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2016SPIE.9905E..6QJ | We present the coating of depthgraded WSi multilayers on the thin glass substrates for telescopes in Xray timing and polarization mission. The multilayer consists of several hundred bilayers in an optimized graded power law design with stringent requirements on uniformity and interface width. We introduce the details of the planar magnetron sputtering facility including the optimization of the deposition process. Results are presented on the uniformity interface width reflectivity and the fabrication of a 200bilayers depth graded multilayer working at hard Xray energies. | 2016-07-01T00:00:00Z | ['2016SPIE.9905E..6QJ', '10.1117/12.2233729'] | null | Multilayer coating of XTP telescope mirrors | 2,016 | 0 | 0.12 | ['PUB_HTML'] | 0 | null |
2024ESS.....560710L | Previous work has established the enhanced occurrence of compact systems of multiple small exoplanets around metalpoor stars. In this talk I will investigate whether the radii distribution between single and multitransiting planets are consistent with being drawn from the same underlying planetary population. We construct a planetary sample of 290 Keplerderived planets orbiting lateK and Mdwarfs containing 149 planets from singletransiting planetary systems and 141 planets from multitransiting compact multiple planetary systems 54 compact multiples. We perform two sample KolmogorovSmirnov tests MannWhitney U tests and AndersonDarling KSampling tests on the radius distributions of our two samples and find statistical evidence p lt 0.0026 that planets in compact multiple systems are larger on average than their singletransiting counterparts. In this talk I will also discuss whether this effect could originate via more efficient outgassing of a secondary atmosphere in compact multiple systems due to the stress and strain forces of interplanetary tides and the amounts of volatiles required in the bulk mantle to account for this result. We discuss the implications that our result has on planet formation theories including the possibility that the planet formation channels for singletransiting and compact multiple planets are different and result in different interior compositions of these planetary populations. | 2024-04-01T00:00:00Z | ['2024ESS.....560710L'] | null | Variations in the Radius Distribution of Single and Compact Multiple Transiting Planets | 2,024 | 0 | 0.32 | ['PUB_HTML'] | 0 | null |
2024ESS.....562717T | We investigate the impact of nongreenhouse gases e.g. N2 CO and O2 on the surface temperatures of Earthlike planets. Nongreenhouse gases are transparent to infrared radiation and do not directly heat the planetary surface. However as nongreenhouse gases become abundant the total atmospheric pressure increases then the absorption lines of greenhouse gases broaden. Consequently the atmosphere absorbs a wider range of infrared wavelengths leading to an indirect warming effect caused by nongreenhouse gases. On the contrary since gas molecules scatter visible light from the host star an increase in total atmospheric pressure may increase the planetary albedo Higher atmospheric pressure decreases energy absorbed by the surface potentially cooling the planetary climate. Wordsworth amp Pierrehumbert 2013 described both cases in which surface temperature can increase and decrease with an increase in atmospheric N2 partial pressure. While changes in surface temperature are qualitatively controlled by which of the warming or cooling effects of nongreenhouse gases is dominant the practical indicator of these two effects remains uncertain. In this study we employ a onedimensional planetary climate model Kasting et al. 1984 to assess the impact of nongreenhouse gases on surface temperatures comprehensively. We conduct parameter surveys on various levels of N2 and CO2 abundance under several host star types and relative humidity models to observe the surface temperature response. We then identify the actual conditions leading to the transition of planetary surface coolingwarming and discuss how nongreenhouse gases control the surface temperature of Earthlike planets. | 2024-04-01T00:00:00Z | ['2024ESS.....562717T'] | null | Revisiting the greenhouse effect of nongreenhouse gases in the atmosphere of Earthlike planets | 2,024 | 0 | 0.29 | ['PUB_HTML'] | 0 | null |
2024ESS.....560702V | In this talk we will present our occurrence rates of shortperiod young planets lt 200 Myr. We conducted a holistic occurrence rate study using both Full Frame Images FFIs and the 2 minute cadence observations from NASAs Transiting Exoplanet Survey Satellite TESS. We sampled over 8000 total stars known to reside in young clusters or associations and recovered 19 planets and candidates including 5 newly identified candidates. We find evidence for both period and radius evolution of planets over the first hundred million years. We find a distinct increase in the occurrence of both Neptune sized planets and planets residing in 10 day orbital periods when compared to the mature age population. Our occurrence rates test the contraction photoevaporation and potentially migration processes that all planets undergo early in their lives. This is the critical timescale by which the intense XUV irradiation from young active host stars is thought to strip planets primordial atmospheres. Comparing the population of planets around young stars against that of their mature counterparts is one avenue to time stamp these processes as they occur. | 2024-04-01T00:00:00Z | ['2024ESS.....560702V'] | null | The occurrence rates of young Neptunesized planets with ages less than 200 Myr | 2,024 | 0 | 0.23 | ['PUB_HTML'] | 0 | null |
2024ESS.....562709A | Planet formation theories predict a relationship between planet mass and metallicity. Abundances measurements may be used to compare to these theoretical expectations if it is assumed that planetary atmospheres are a closed box whose elemental abundances reflect the time of formation. However if there is ongoing accretion of heavy elements then the abundances may instead partially reflect those of the heavy element reservoir as well as those of the primordial planet. Accretion of interplanetary dust is of interest as it may act as a steady source of heavy elements in the upper atmosphere over long timescales. If the accretion rate is large enough this accreted dust and ablated gasphase atoms may generate significant opacity possibly to the point of affecting the transmission spectrum. In this talk I will discuss observational constraints on interplanetary dust orbiting near the parent star as well as theoretical estimates for the efficiency of accretion of this dust by extrasolar planets. Dust particles inspiraling toward the star due to PoyntingRobertson drag will encounter meanmotion resonances with the starplanet binary and will suffer one of three fates when they exit resonance hitting the planet hitting the star or being ejected from the system. Results will be presented that show the fraction of dust hitting the planet can be surprisingly high 10s of percent hence much of the inspiraling dust may end up polluting the planetary upper atmosphere. Results for model transmission spectra including accreted dust will be presented. | 2024-04-01T00:00:00Z | ['2024ESS.....562709A'] | null | The Sky is Falling On Exoplanets | 2,024 | 0 | 0.37 | ['PUB_HTML'] | 0 | null |
2023plat.confE..25M | Stars that have precise accurate and independent measurements of their fundamental properties will be essential to quantify the precision and accuracy of stellar parameters in the PLATO data products. The benchmark stars work package WP125500 have identified several types of star that will be useful for benchmarking PLATO data products e.g. eclipsing binaries transiting hot Jupiter systems nearby stars with directly measured angular diameters etc. In this talk I will review the different types of benchmark star and give some preliminary results for the number and properties of benchmark stars in the LOPN1 and LOPS2 fields. | 2023-06-01T00:00:00Z | ['2023plat.confE..25M', '10.5281/zenodo.8106039'] | ['Zenodo community pssc23'] | Benchmark stars in the PLATO LOP fields | 2,023 | 0 | 0.24 | ['PUB_HTML'] | 0 | null |
2023pimo.conf...96L | For meteor showers the observed activity based on the raw counts of meteor echoes recorded by a radio forward scatter system is modulated by the position of the radiant throughout the day and does not truly reflect the real activity of the shower. A possibility to correct these raw counts is to compute the socalled Observability Function OF which contains a geometrical part and a sensitivity part. In this paper we recall the most important characteristics of the OF described in Verbeeck 1997 and discuss them in the context of the BRAMS forward scatter network. We conclude with future activities on how to apply the OF to the raw counts of a few main meteor showers obtained from the Citizen Science project the Radio Meteor Zoo. | 2023-01-01T00:00:00Z | ['2023pimo.conf...96L'] | null | Observability Function of the BRAMS network | 2,023 | 0 | 0.17 | ['ADS_PDF', 'ADS_SCAN'] | 0 | null |
2023EGUGA..2514102S | The variability of the upper atmosphere is largely influenced by dynamical forcing from the lower and middle atmosphere. The Mesosphere and Lower Thermosphere MLT is the transition region between the middle atmosphere and the upper atmosphere and it determines dynamical forcing to the upper atmosphere from below. It is thus of high importance to know describe and understand the dynamical processes within the MLT to quantify dynamics. Therein General Circulation Models GCMs have been a significant tool to explain MLT processes.However developing the right parameterizations that allow to accurately model neartorealistic states of the MLT by GCMs is challenging which is reflected in a large diversity of results from different models in comparison to observations e.g. of winds and temperatures at the MLT.In recent years the community model ICON Icosahedral Nonhydrostatic Weather and Climate Model has been expanded into altitudes up to 150 km named the UA Upper Atmosphere branch. UAICON is increasingly being applied to model and to understand MLT processes and how they are controlled by the lower and middle atmosphere.We present newly developed capabilities of UAICON. Examples are mesospheric cooling during stratospheric warming events low summer mesopause temperatures through appropriate specification of gravity wave parameterizations and runs of high spatial resolution. Results are discussed in comparison with observations and with predictions by other GCMs. | 2023-05-01T00:00:00Z | ['2023EGUGA..2514102S', '10.5194/egusphere-egu23-14102'] | null | Dynamics and variability of the MLT represented by UAICON | 2,023 | 0 | 0.16 | ['PUB_HTML', 'PUB_PDF'] | 0 | null |
2023EGUGA..2514084B | Previous studies have found that highenergy radiation like cosmic rays and stellar energetic particles can induce the initial nucleation of cloud particles from molecular clusters but the effect on larger existing particles is still poorly understood. This study explores the question How is the aggregation of mineral cloud particles affected by highenergy radiation and humidity. We present experiments conducted in an atmosphere chamber on the charging and aggregation of 50nm SiO2 particles under varying degrees of gamma radiation and relative humidity. We observe an aggregation of the SiO2 particles to form larger clusters and that this aggregation is inhibited by irradiation with gamma radiation. We find that nonirradiation SiO2 particles are generally more positively charged in comparison to a bipolar charge distribution and that gamma radiation shifts the particles to a more negative charge. The effect of gamma radiation on the aggregation and charge of the particles is present both at lower 20 and higher 60 relative humidity. When varying the relative humidity from 20 to 80 we find no significant direct effect of relative humidity on the aggregation of the particles. These results are presented and discussed in relation to previous studies of nucleation and condensation. In recent years exoplanet research has focused on how we can interpret atmosphere observations through models and here cloud formation has proven to be a challenge. Clouds are known to play a role in both the energy balance and chemistry of atmospheres as well as directly affecting the spectrum observed from a planet. Exoplanet clouds are believed to be very chemically heterogeneous and SiO2 is one of the species that easily condense making SiO2 relevant both as a nucleation seed on Earthlike planets and as a cloud species on Exoplanets. Since cloud formation has been found to be affected not only by the atmospheric properties but also by highenergy radiation from outside the atmosphere it indicates that the host star and interstellar environment of an exoplanet might affect its clouds. | 2023-05-01T00:00:00Z | ['2023EGUGA..2514084B', '10.5194/egusphere-egu23-14084'] | null | Aggregation and charging of mineral cloud particles underhighenergy irradiation | 2,023 | 0 | 0.22 | ['PUB_HTML', 'PUB_PDF'] | 0 | null |
2023EGUGA..2513871T | The Tharsis Region has been an interest of study for many years due to its large impact on the long wavelength gravity field and topography of Mars. The leading theory on the origin of the volcanic region is a combination of both isostatic flexure of a thickened crust and a small contribution due to a possible large superplume residing in the upper mantle. The isostatic balance on which previous studies have relied does not adequately explain the longwavelength gravity field spectra. These longwavelength signals contribute to large scale features in the mantle. We consider the presence of a dynamic mass anomaly below the Tharsis Region. This could help explain the geological surveys of the relative young lava flows. By looking at mantle dynamic models we can explore the effect of a superplume that is actively rising in the mantle and changing the geoid over time. We ran a series of instantaneous axisymmetric finite element models of Mars with varying plume and subsurface structural variables constrained by InSight. We run the model for 50 years thereby accounting for the total duration of satellite data acquisition. The deformation in the model allows us to calculate the change in dynamic topography and gravity anomaly.Our preliminary results show dynamic topography rates of a few centimetres per year and gravity rates in the order of 0.1 Gal per year. These gravity rates should fall within the precision of the Mars Reconnaissance Orbiter gravity field estimates but are masked by other geological surface mass changes. Our results show that with longer and dedicated gravity observations we should be able to observe the large scale mantle dynamics of Mars. | 2023-05-01T00:00:00Z | ['10.5194/egusphere-egu23-13871', '2023EGUGA..2513871T'] | null | The changing gravity field due to a superplume under the Tharsis Region | 2,023 | 0 | 0.06 | ['PUB_HTML', 'PUB_PDF'] | 0 | null |
2016SPIE.9904E..2XT | The Transiting Exoplanet Survey Satellite TESS is an Explorerclass mission dedicated to finding planets around bright nearby stars so that more detailed followup studies can be done. TESS is due to launch in 2017 and careful characterization of the detectors will need to be completed on ground before then to ensure that the cameras will be within their photometric requirement of 60ppmhr. TESS will fly MITLincoln Laboratories CCID80s as the main scientific detector for its four cameras. They are 100m deep depletion devices which have low dark current noise levels and can operate at low light levels at room temperature. They also each have a frame store region which reduces smearing during readout and allows for near continuous integration. This paper describes the hardware and methodology that were developed for testing and characterizing individual CCID80s. A dark system with no stimuli was used to measure the dark current. FeSUP55SUP and CdSUP109SUP Xray sources were used to establish gain at low signal levels and its temperature dependence. An LED system that generates a programmable series of pulses was used in conjunction with an integrating sphere to measure pixel response nonuniformity PRNU and gain at higher signal levels. The same LED system was used with a pinhole system to evaluate the linearity and charge conservation capability of the CCID80s. | 2016-07-01T00:00:00Z | ['10.1117/12.2232886', '2016SPIE.9904E..2XT'] | null | Testing and characterization of the TESS CCDs | 2,016 | 0 | 0.17 | ['PUB_HTML'] | 2 | null |
2024CoTPh..76j5402Y | This study focuses on the effects of a polytropic fluid on a charged gravitational source within fT gravity where T is the torsion scalar. We investigate how the electromagnetic field affects the flow of energy in spherically symmetric and static celestial objects that contain relativistic fluids. By using the gravitational decoupling technique we analyze the effects of polytropic fluid on the dynamics of the gravitational source accompanied by the matching of the interior geometry with an exterior at the hypersurface . Finally with the help of the Tolman solution we observe the conduct of energy conditions with the existence of charge using fT field equations and got the intended outcomes. | 2024-10-01T00:00:00Z | ['10.1088/1572-9494/ad5b4d', '2024CoTPh..76j5402Y'] | ['complexity', 'hydrodynamics', 'anisotropy', 'self-gravitating systems', 'energy exchange'] | Energy exchange between charged relativistic fluids in fT gravity | 2,024 | 0 | 0.16 | ['PUB_HTML'] | 0 | null |
2024E&SS...1103088G | Previous studies that intercompared global Level4 L4 sea surface temperature SST analyses were centered on the assessment of the accuracy and bias of SST by comparing them with independent nearsurface Argo profile temperature data. This type of assessment is centered on the absolute value of SST rather than on SST spatial properties gradients which is more relevant to the study of oceanographic features e.g. fronts eddies etc. and ocean dynamics. Here we use for the first time the spectrum of singularity exponents to assess the structural and dynamical quality of different L4 gapfilled products based on the multifractal theory of turbulence. Singularity exponents represent the geometrical projection of the turbulence cascade and its singular spectrum can be related to the probability density function of the singularity exponents normalized by the scale. Our results reveal that the different schemes used to produce the L4 SST products generate different singularity spectra which are then used to identify a potential loss of dynamical information or structural coherence. This new diagnostic constitutes a valuable tool to assess the structural quality of SST products and can support data satellite SST producers efforts to improve the interpolation schemes used to generate gapfilled SST products. | 2024-10-01T00:00:00Z | ['10.1029/2023EA003088', '2024E&SS...1103088G'] | ['L4 SST intercomparison', 'SST analysis', 'dynamical quality assessment', 'feature fidelity', 'turbulence'] | Structural and Dynamical Quality Assessment of GapFilled Sea Surface Temperature Products | 2,024 | 0 | 0.19 | ['PUB_HTML'] | 0 | null |
2016SPIE.9904E..1FA | Pursuing ground breaking science in a highly costconstrained environment presents new challenges to the development of future space astrophysics missions. Within the conventional cost models for large observatories executing a flagship mission after next appears to be unsustainable. To achieve our nations science ambitions requires not a paradigm shift but a completely new paradigm of system design development and manufacture. This paper explores the nature of the current paradigm and proposes a series of steps to guide the entire community to a sustainable future. | 2016-07-01T00:00:00Z | ['2016SPIE.9904E..1FA', '10.1117/12.2234492'] | null | Ensuring the enduring viability of the space science enterprise new questions new thinking new paradigms | 2,016 | 0 | 0 | ['PUB_HTML'] | 0 | null |
2016cosp...41E.841H | Solar Sail is a kind of spacecraft that can achieve extremely high velocity by light pressure instead of chemical fuel. The great accelerate rely on its high areatomass ratio. So solar sail is always designed in huge size and it use ultra thin and light weight materials. For 100meter class solar sail two key points must be considered in the design process. They are folddeployment method and material property change in space environment. To test and verify the folddeployment technology a 88m principle prototype was developed. Sail membrane folding in method of IKAROS NanosailD and new proposed Lshape folding pattern were tested on this prototype. Their deployment properties were investigated in detail and comparisons were made between them. Also the space environment suitability of ultra thin polyimide films as candidate solar sail material was analyzed. The preliminary test results showed that membrane by all the folding method could deploy well. Moreover sail membrane folding by Lshape pattern deployed more rapidly and more organized among the three folding pattern tested. The mechanical properties of the polyimide had no significant change after electron irradiation. As the preliminary research on the key technology of solar sail spacecraft in this paper the results of the study would provide important basis on largescale solar sail membrane select and folddeploying method design. | 2016-07-01T00:00:00Z | ['2016cosp...41E.841H'] | null | Ground Deployment Demonstration and Material Testing for Solar Sail | 2,016 | 0 | 0.24 | null | 0 | null |
2016apra.prop...75P | The prime objective of the proposed work is to clarify the origin of Galactic cosmic rays through analysis and interpretation of experimental data on cosmic ray energy spectra and composition obtained in balloon spacecraft and ground based experiments. This study will include modelling of cosmic ray acceleration and propagation in the Galaxy over a wide energy range from the lowest energies about a few MeV where direct measurements were performed in the Voyager 1 mission and up to energies gt1017 eV where transition from Galactic to extragalactic components in the spectra observed at Earth most likely occurs. The proposed investigation is based on current theoretical concepts and the results of contemporary experiments in cosmic ray physics. Energy spectra of cosmic ray primary and secondary nuclei shaped by cosmic ray diffusion in the interstellar medium will be calculated and compared with spectra observed at Earth. Cosmic ray transport and acceleration in a selfconsistent model of Galactic wind driven by cosmic ray pressure will be explored. The central topic of the proposed investigation is interpretation of anomalies in cosmic ray energy spectra such as deviations from a plain power law and spectral hardening above 230 GV. It also includes different slopes of proton and helium spectra bending of cosmic ray spectra at energies below a few GeVn spectral and elemental peculiarities in the knee region and transition to the extragalactic component in the observed cosmic rays. The study of cosmic accelerators supports the Science Mission Directorates Goal for Astrophysics in NASAs 2010 Science Plan Discover how the universe works explore how the universe began and evolved and search for Earthlike planets. It specifically addresses the Science Question How do matter energy space and time behave under the extraordinarily diverse conditions of the cosmos | 2016-01-01T00:00:00Z | ['2016apra.prop...75P'] | null | Investigation of Cosmic Ray Acceleration and Propagation at Energies from MeV to the Energy Limit of Galactic Accelerators | 2,016 | 0 | 0 | null | 0 | null |
2024IAUGA..32P1784R | Pulsar Timing Arrays are now reaching sensitivity towards detecting angular spatial correlations described by Hellings and Downs HD curve as expected from binary mergers of a cosmic population of Super Massive Black Hole Binaries. The remarkable sensitivity of the MeerKAT telescope has enabled the detection of HD curve in MeerKAT Pulsar Timing Array MPTA dataset spanning around 5 years. This HD signature results from the expected quadrupolar nature of the Gravitational Wave Background GWB specifically the h and hx polarisation modes. In this work we investigate alternative GW polarisation modes known as the Scalar Transverse ST modes along with the h and hx modes and consider the sensitivity of the MPTA and future Square Kilometre Array SKA datasets to these Scalar Transverse ST modes. This provides an excellent test for modified gravity theories. We will present our preliminary results using the MPTA dataset and simulations. | 2024-08-01T00:00:00Z | ['2024IAUGA..32P1784R'] | null | Search for alternative GW polarisation modes in the MeerKAT Pulsar Timing Array data. | 2,024 | 0 | 0.33 | ['PUB_PDF'] | 0 | null |
2024JDE...409..136Y | In this paper we classify the solutions of the following elliptic equation in mmlmath altimgsi1.svgmmlmsubsupmmlmrowmmlmi mathvariantdoublestruckRmmlmimmlmrowmmlmrowmmlmo linebreakbadbreak linebreakstyleaftermmlmommlmrowmmlmrowmmlmn4mmlmnmmlmrowmmlmsubsupmmlmathmmlmath altimgsi2.svgmmlmrowmmlmo stretchytruemmlmommlmsupmmlmrowmmlmo stretchyfalsemmlmommlmommlmommlmi mathvariantnormalmmlmimmlmo stretchyfalsemmlmommlmrowmmlmrowmmlmn2mmlmnmmlmrowmmlmsupmmlmiummlmimmlmo stretchyfalsemmlmommlmixmmlmimmlmo stretchyfalsemmlmommlmommlmommlmsupmmlmrowmmlmiemmlmimmlmrowmmlmrowmmlmn4mmlmnmmlmiummlmimmlmo stretchyfalsemmlmommlmixmmlmimmlmo stretchyfalsemmlmommlmrowmmlmsupmmlmspace width1emmmlmspacemmlmrowmmlmi mathvariantnormalinmmlmimmlmrowmmlmspace width0.25emmmlmspacemmlmsubsupmmlmrowmmlmi mathvariantdoublestruckRmmlmimmlmrowmmlmrowmmlmommlmommlmrowmmlmrowmmlmn4mmlmnmmlmrowmmlmsubsupmmlmommlmommlmfracmmlmrowmmlmommlmommlmiummlmimmlmrowmmlmrowmmlmommlmommlmimmlmimmlmrowmmlmfracmmlmommlmommlmn0mmlmnmmlmspace width1emmmlmspacemmlmrowmmlmi mathvariantnormalonmmlmimmlmrowmmlmspace width0.25emmmlmspacemmlmommlmommlmsubsupmmlmrowmmlmi mathvariantdoublestruckRmmlmimmlmrowmmlmrowmmlmommlmommlmrowmmlmrowmmlmn4mmlmnmmlmrowmmlmsubsupmmlmommlmommlmfracmmlmrowmmlmommlmommlmo stretchyfalsemmlmommlmommlmommlmi mathvariantnormalmmlmimmlmiummlmimmlmo stretchyfalsemmlmommlmrowmmlmrowmmlmommlmommlmimmlmimmlmrowmmlmfracmmlmommlmommlmsupmmlmrowmmlmiemmlmimmlmrowmmlmrowmmlmn3mmlmnmmlmiummlmimmlmrowmmlmsupmmlmspace width1emmmlmspacemmlmrowmmlmi mathvariantnormalonmmlmimmlmrowmmlmspace width0.25emmmlmspacemmlmommlmommlmsubsupmmlmrowmmlmi mathvariantdoublestruckRmmlmimmlmrowmmlmrowmmlmommlmommlmrowmmlmrowmmlmn4mmlmnmmlmrowmmlmsubsupmmlmo.mmlmommlmrowmmlmath Under some assumptions we will show that on the boundary of mmlmath altimgsi1.svgmmlmsubsupmmlmrowmmlmi mathvariantdoublestruckRmmlmimmlmrowmmlmrowmmlmo linebreakbadbreak linebreakstyleaftermmlmommlmrowmmlmrowmmlmn4mmlmnmmlmrowmmlmsubsupmmlmath the solutions must have the following formmmlmath altimgsi26.svgmmlmiummlmimmlmo stretchyfalsemmlmommlmsupmmlmrowmmlmixmmlmimmlmrowmmlmrowmmlmommlmommlmrowmmlmsupmmlmommlmommlmn0mmlmnmmlmo stretchyfalsemmlmommlmo linebreakbadbreak linebreakstyleaftermmlmommlmi mathvariantnormallnmmlmimmlmommlmommlmfracmmlmrowmmlmiCmmlmimmlmo stretchyfalsemmlmommlmimmlmimmlmo stretchyfalsemmlmommlmrowmmlmrowmmlmsupmmlmrowmmlmimmlmimmlmrowmmlmrowmmlmn2mmlmnmmlmrowmmlmsupmmlmo linebreakbadbreak linebreakstyleaftermmlmommlmo stretchyfalsemmlmommlmsupmmlmrowmmlmixmmlmimmlmrowmmlmrowmmlmommlmommlmrowmmlmsupmmlmo linebreakbadbreak linebreakstyleaftermmlmommlmsubsupmmlmrowmmlmixmmlmimmlmrowmmlmrowmmlmn0mmlmnmmlmrowmmlmrowmmlmommlmommlmrowmmlmsubsupmmlmsupmmlmrowmmlmo stretchyfalsemmlmommlmrowmmlmrowmmlmn2mmlmnmmlmrowmmlmsupmmlmrowmmlmfracmmlmommlmommlmath where C is a positive constant depending only on and mmlmath altimgsi27.svgmmlmsubsupmmlmrowmmlmixmmlmimmlmrowmmlmrowmmlmn0mmlmnmmlmrowmmlmrowmmlmommlmommlmrowmmlmsubsupmmlmath is a fixed point on mmlmath altimgsi6.svgmmlmommlmommlmsubsupmmlmrowmmlmi mathvariantdoublestruckRmmlmimmlmrowmmlmrowmmlmo linebreakbadbreak linebreakstyleaftermmlmommlmrowmmlmrowmmlmn4mmlmnmmlmrowmmlmsubsupmmlmath. | 2024-11-01T00:00:00Z | ['2024JDE...409..136Y', '10.1016/j.jde.2024.06.037'] | ['35J60', '35J57', '35J15', 'Elliptic equation', 'Moving spheres method', 'Half space'] | Classification of solutions for some higher order elliptic equations in half space | 2,024 | 0 | 0.17 | ['PUB_HTML'] | 0 | null |
2024IAUGA..32P1018O | This research investigates instability of the inplane equilibrium points EPs of the restricted threebody problem with PoyntingRobertson PR drag force and variable masses. The motion of the primaries and their mass variation is governed by the GyldenMestschersky problem GMP and unified Mestschersky law UML respectively under the conditions that both primaries are radiation emitters with PR drag. The dynamical equations are derived and it is seen that a pair of triangular equilibrium points TEPs which are defined by the mass parameter radiation pressure and PR drag force. The stability of the inplane EPs is investigated analytically and numerically for a dust grain particle and it is seen that all the EPs are unstable. The PR drag is a strong perturbing force which changes stability to instability and motion around the EPs are unstable in the presence of the PR drag. Additionally we explore the zero velocity curves around the inplane EPs and our results show that the radiation pressure and PR drag increase the region where motion of the dust grain is dynamically allowed around the TEPs though this influence is very minimal. Also it is seen that as the mass parameter increases the energy constant also increases thus increasing the region where motion of the dust grain is permissible. The stability of the inplane EPs of the nonautonomous system which differ from those of the autonomized system by a function of time are unstable. | 2024-08-01T00:00:00Z | ['2024IAUGA..32P1018O'] | null | Inplane Instability Equilibrium Points of the Restricted ThreeBody Problem with PR Drag and Variable Masses | 2,024 | 0 | 0.16 | ['PUB_PDF'] | 0 | null |
2024IAUGA..32P2209N | In many places in Africa particularly in rural Africa Astronomy is seen as an exotic science belonging to the West. To address this misconception and make Astronomy more relatable Elimisha Msichana Elimisha Jamii na Astronomia EMEJA organised a workshop in Kitale Kenya targeting high school teachers and the locals. The objective was to discuss and document Astronomy application and stories in the African context from back in time. For example what were the cultural beliefs with regards to creation of the Universe Different communities in Kenya have different ideas and beliefs on how the Universe the earth the sun stars and moon were created. Our target audience were diverse and coming from different communities and therefore provided diverse Astronomyrelated tales that were nicely documented. Here I will share some of these tales. For example the Kikuyus believed that all the demons were sent to irima iruku Kikuyu for a bottomless hole where they could never escape. This being a likely reference to a black hole. The aim was to build upon these reflections and to use the ideas generated to effectively deliver Astronomyrelated content in classrooms as part of the curriculumn for secondary education in Kenya. Overall we aimed to spur interest in and appreciation of Astronomy across the whole community. | 2024-08-01T00:00:00Z | ['2024IAUGA..32P2209N'] | null | Short stories A Collection of African Astronomy Tales. | 2,024 | 0 | 0.16 | ['PUB_PDF'] | 0 | null |
2013SPPhy.148...45M | Stars twinkle because their light propagates through the atmosphere. The same phenomenon is expected when the light of remote stars crosses a Galactic disk or halo refractive medium such as a molecular cloud ltCitationRef CitationIDCR1gt1 ltCitationRef CitationIDCR5gt5. We present the promising results of a test performed with the ESONTT and the perspectives. | 2013-01-01T00:00:00Z | ['10.1007/978-94-007-7241-0_6', '2013SPPhy.148...45M'] | ['Physics'] | Search for Turbulent Gas Through Interstellar Scintillation | 2,013 | 0 | 0.06 | ['PUB_HTML'] | 0 | null |
2016RoAJ...26...77T | The CCD observations of mutual events in the system of Galilean satellites of Jupiter have been carried out in the period of January 2015 to May 2015 at ClujNapoca Astronomical Observatory using two observing instruments. During PHEMU 2015 Campaign we obtained useful photometric observations for 17 phenomena 6 occultations and 11 eclipses. Some preliminary results using extended cubic spline fitting functions are given. | 2016-01-01T00:00:00Z | ['2016RoAJ...26...77T'] | null | PHEMU 2015 Campaign at Astronomical Observatory ClujNapoca | 2,016 | 0 | 0.16 | ['PUB_PDF'] | 0 | null |
2016RoAJ...26...57B | The paper presents first technical realizations of a mobile platform for vertical deviation determination at a satisfactory precision and low cost. The conception of the platform was made in the framework of a project regarding CCD astrogeodetic vertical deviation for geoid determination or geoid modeling. The project with the acronym AGEO represents a collaboration between Technical University of Civil Engineering Bucharest Faculty of Geodesy TUCEBFG Astronomical Institute of the Romanian academy AIRA and a private partner GeoGIS Proiect S.R.L. The paper presents some hardware and software aspects regarding design development and automation of the platform based on an electrooptical geodetic instrument CCD observations and satellite time synchronization for astrogeodetic measurements. | 2016-01-01T00:00:00Z | ['2016RoAJ...26...57B'] | null | Astrogeodetic platform for high accuracy geoid determinat ion | 2,016 | 0 | 0.19 | ['PUB_PDF'] | 0 | null |
2016SPIE.9906E..6FC | The narrowband phasing algorithm that was originally developed at Keck has largely been replaced by a broad band algorithm that although it is slower and less accurate than the former has proved to be much more robust. A systematic investigation into the lack of robustness of the narrowband algorithm has shown that it results from systematic errors of order 20 nm that are wavelengthdependent. These errors are not wellunderstood at present but they do not appear to arise from instrumental effects in the Keck phasing cameras or from the segment coatings. This leaves high spatial frequency aberrations or scattering within 60 mm of the segment edges as the most likely origin of the effect. | 2016-07-01T00:00:00Z | ['2016SPIE.9906E..6FC', '10.1117/12.2230748'] | null | Phasing the segments of the Keck and Thirty Meter Telescopes via the narrowband phasing algorithm chromatic effects | 2,016 | 0 | 0.14 | ['PUB_HTML'] | 0 | null |
2016RoAJ...26...25B | The article presents results of several years of observing runs devoted to NearEarth Asteroids NEAs. Astrometry of NEAs was provided either for secure orbits of newly discovered objects or to decrease the uncertainty in orbital elements. Photometry and spectroscopy could be associated to astrometry in order to constrain physical and mineralogical properties of NEAs. Of a crucial importance into as successful run is the manner on which the observations are scheduled during each night and over the observational list. While the adhoc list is created the balance between several dynamical parameters are very important for the strategy of observations. | 2016-01-01T00:00:00Z | ['2016RoAJ...26...25B'] | null | Observations for Secure and Recovery NearEarth Asteroids | 2,016 | 0 | 0.16 | ['PUB_PDF'] | 2 | null |
2024Icar..41316011C | Cuzzi et al. 2014 described the dynamical properties of Saturns F Ring region numerically and analytically. They found that most of the region was dynamically chaotic due to repeated encounters with the very eccentric shepherding moons Prometheus and Pandora making the longterm stability of the F ring hard to understand. However they did discover relatively stable clusters of particles at a set of narrow regularly spaced radial locations near to firstorder Lindblad resonances. One of these is close to the observed semimajor axis of Saturns F Ring based on stellar occultation and imaging observations. Being unable at the time to distinguish Corotational and Lindblad resonances CRs and LRs they focused their discussion on what they thought was a new kind of dynamical cancellation they dubbed antiresonances lying very close to the numerically detected stable zones that might be preventing the dynamical chaos from rising near these narrow radial zones. Here we report an error in their analytical development of the locations of the antiresonances that renders that hypothesis irrelevant and describe the source of the error. We also present updated long integrations that clarify the longevity of particles in stable locations noting some labeling errors in our previous plots. Recently Cuzzi et al. 2023 have shown that the F ring is anchored by a series of discontinuous arcs of relatively large particles dominating its mass that orbit in one specific CR with Prometheus. They describe why the CR is at least partly responsible for the stability of the F Ring but it remains a puzzle why it is the only such CR stably populated in such a way especially because it actually seems to be less stable than several near neighbors. | 2024-05-01T00:00:00Z | ['10.1016/j.icarus.2024.116011', '2024Icar..41316011C'] | ['Planetary rings', 'Saturn', 'Rings', 'Resonances', 'Orbital', 'Celestial mechanics'] | Corrigendum to Saturns F Ring core Calm in the midst of chaos Icarus 232 April 2014 157175 | 2,024 | 0 | 0.35 | ['PUB_HTML'] | 1 | null |
2024Icar..41015893C | Eistla Regio Venus is a locus of major plumegenerated magmatism and tectonics. We focus on the central portion termed Central Eistla Regio. More than 19000 extensional lineaments grabens fissures and fractures were mapped in the area 1326E 010N at 1500000 scale using full resolution Magellan SAR radar images. These structures are interpreted to represent the surface expression of underlying mafic dykes and have been grouped on the basis of trend into radiating circumferential and linear dyke swarms. Thirtytwo swarms are identified and linked to 20 magmatic centres most of which are located within or near two coronae Beletili and Gaia Gaya coronae while others are linked to magmatic centres outside the study area. These magmatic centres are interpreted to be linked to underlying mantle plumes and the sizes of the underlying flattened plume heads are estimated from the interpreted dyke swarms for radiating swarms the radius of the transition from proximal radiating to more distal linear pattern and for circumferential dykes the radial distance to the outer boundary of the circumferential pattern. Plume heads for the largest centres Beletili and Gaia coronae are estimated at about 230 km and 275 km in radius respectively. These sizes are less than the 1200 km radii predicted for a plume arriving from the deep mantle and would suggest an origin at a shallower level likely a midmantle boundary i.e. between upper and lower mantle. The NW alignment of Beletili and Gaia corona and other magmatic centres in our study area potentially represents structural control by a rift zone which can be traced further north to Anala Mons one of two main plume centres of Central Eistla Regio. | 2024-03-01T00:00:00Z | ['10.1016/j.icarus.2023.115893', '2024Icar..41015893C'] | ['Central Eistla Regio', 'Mapping of grabens', 'Dyke swarms', 'Magmatic plume centres', 'Belet-Ili Corona', 'Venus', 'Gaia corona'] | Dyke swarm history in Beletili and Gaia Gaya Coronae Region 1326E 010N Central Eistla Regio Venus | 2,024 | 0 | 0.23 | ['PUB_HTML'] | 1 | null |
2024Icar..41015885J | Due to the lack of insitu geotechnical data from lunar Permanently Shadowed Regions PSRs it is important that a versatile icy regolith simulant be used in terrestrial development of rovers excavators and water extractors intended for operating in lunar PSRs. Fine tuning of existing icy regolith simulant properties is not possible for a given water percentage they either exhibit strength similar to high strength concrete or to sand but nothing in between. In this work we present a novel method for creating icy lunar regolith simulant called Pressure Sintered icy lunar regolith Simulant. PSS is notable for being created from solid phase water and for being tailorable to a wide range of mechanical properties through the sintering of ice and regolith grains induced by applied uniaxial pressure. Samples were produced at 0 2 5 and 10 ice content as measured by weight and were pressed at four different pressure levels. Penetration resistance was measured for each of these samples and it was observed that a continuous distribution of penetration resistance levels could be achieved by varying the applied pressure and ice content. Significant relaxation of samples during the pressing process was also observed. The production method for PSS is included and is followed by the penetration resistance and density results along with some qualitative observations. Finally we make recommendations for the use of PSS in terrestrial testing activities. | 2024-03-01T00:00:00Z | ['10.1016/j.icarus.2023.115885', '2024Icar..41015885J'] | ['Regoliths', 'Ices', 'Mechanical properties', 'Moon', 'Surface'] | Pressure Sintered icy lunar regolith Simulant PSS A novel icy regolith simulant production method | 2,024 | 0 | 0.24 | ['PUB_HTML'] | 0 | null |
2024Icar..41015873T | The surface of Europa is heavily irradiated by highenergy particles with the energy ranges of 1100 MeV for primary electrons and 10 keV for secondary electrons. These irradiations may cause oxidation of surface materials such as chlorides and sulfurbearing species through reactions with oxidative radicals formed by dissociation of HSUB2SUBO ice. Similar irradiationinduced oxidation could have occurred in nearsurface ice on Mars. However most of previous experiments simulated 10 keV electron irradiation onto ice materials on Europa and Mars and few studies have investigated the oxidation of chlorides and sulfur by MeV electron irradiation. Here we performed laboratory experiments on MeV electron irradiation as well as 10 keV electron and UV irradiations onto mixtures of HSUB2SUBO ice and chlorides or elemental sulfur at low temperatures. Our experimental results indicate selective oxidation of sulfur against chlorides with negligible formation of oxychlorides on irradiation of HSUB2SUBO ice and chloride mixtures regardless of experimental conditions temperature electron energy or presence of oxidants in ice. Sulfate is effectively formed by the electron irradiation. This selective oxidation may be caused by the different stabilities of atoms within irradiated HSUB2SUBO ice. If sulfate on Europas surface is transported into the subsurface ocean this could provide energy sources for possible chemoautotrophic life in the ocean. On Europa sulfur would be one of key elements in redox chemistry on the surface and possibly in the subsurface ocean. | 2024-03-01T00:00:00Z | ['10.1016/j.icarus.2023.115873', '2024Icar..41015873T'] | ['Europa', 'Mars', 'Ice composition', 'Surface processes', 'Laboratory astrophysics'] | Comparing the radiolytic oxidation of sulfur and chloride within ice on Europa and Mars | 2,024 | 0 | 0.35 | ['PUB_HTML'] | 0 | null |
2024Icar..41716117F | The diurnal and seasonal variations of orographic water ice clouds in the Tharsis region have been investigated with EXI observations for MY 36 and 37. In order to provide context meteorological fields from the Mars PCM Mars Planetary Climate Model led by Laboratoire de Mtorologie Dynamique Paris France have been incorporated. These fields include water ice column atmospheric temperature meteorological winds water vapor and dust mixing ratio. The diurnal cycle has been studied for sunlit hours 6 am6 pm by sampling data into 5 local time bins. Both the EXI observations and the Mars PCM underscore the significant role plays by diurnal thermal tides in controlling the thickness and existence of water ice clouds in the Tharsis region. During Spring and Summer water ice clouds form in the morning and lateafternoon hours and exhibit greater thickness compared to those that form during the afternoon primarily due to the influence of thermal tides. During Fall and Winter water ice clouds are typically observed in the Arsia Mons region occasionally extending to the Pavonis Mons region. During the Fall and Winter seasons the clouds that form are mostly thin and have a tendency to develop in the afternoon hours while the morning hours typically remain cloudfree or exhibit extremely thin clouds. This phenomenon can be attributed to a combination of factors including the existence of cold temperature zones at higher altitudes formed by the influence of strong trade winds and the impact of diurnal thermal tides. According to the Mars PCM water ice clouds typically form at altitudes below 25 km during Spring and Summer whereas during Fall and Winter cloud formation occurs at altitudes above 25 km. | 2024-07-01T00:00:00Z | ['10.1016/j.icarus.2024.116117', '2024Icar..41716117F'] | ['Mars', 'Water ice clouds', 'EMM/EXI', 'The Mars PCM', 'Tharsis region'] | Diurnal and seasonal variations of orographic clouds in the Tharsis region with EMMEXI observations and the Mars Planetary Climate Model | 2,024 | 0 | 0.34 | ['PUB_HTML'] | 1 | null |
2024E&PSL.64418922L | Numerous potential landslides with slow sliding speeds pose a continuous threat to human safety. The movements of these landslides continuously modify hydrogeological conditions and lead to cracks expansion making it easier for subsequent rainfall to infiltrate into the landslide interior. Monitoring the tiny variations of structures and porewater pressure in the interior of landslides can help understanding this coupling mechanism and accessing landslide damage risk. Here we utilized seismic ambient noise interferometry to assess hourly velocity changes that enable us to quantify the response of landslides to external factors at different depths including earthquakes rainfall and mechanical effects from sliding. In a case of Xishan Village Landslide Sichuan Province China we observed an outstanding velocity drop coinciding with the onset of rainfall and bursts in tremor activity in a period in which the landslide experienced vertical displacement. Our observations highlight the new sight to investigate how the mechanical process of landslide movement modifies hydrogeological conditions and promotes rainfall infiltration as well as assesses the subsequent recovery process. | 2024-10-01T00:00:00Z | ['2024E&PSL.64418922L', '10.1016/j.epsl.2024.118922'] | ['Ambient noise', 'Seismic velocity change', 'Landslide', 'Rainfall', 'Hydrogeological condition change'] | Monitoring crack opening via seismic velocity variation to assess that fatal effect of precipitation for landslide motion | 2,024 | 0 | 0.28 | ['PUB_HTML'] | 0 | null |
2024E&PSL.64418919W | Investigating the presentday pattern of strain accumulation along the Altyn Tagh fault ATF in northwestern Tibet is critical for our broader understanding of deformation around large active strikeslip faults and the associated seismic hazards. Previous geodetic and geological studies show an eastward decrease of slip rate along the centraleastern ATF but the spatial variation of the slip rates and the mechanism causing such variation are uncertain. Additionally interseismic deformation around the restraining bends along the ATF and its pattern of termination towards its eastern end are also unclear. Here we derive surface velocities and strain rates around the centraleastern ATF system using Sentinel1 and GNSS velocities. We estimate fault parameters including slip rate and locking depth for the ATF and other related active faults indicated by our strain rate maps using a Bayesian inversion approach. Our results show shear strain is mainly concentrated on the ATF between 86E and 95E. The strikeslip rate of the ATF remains constant at 8 mmyr between 86E and 90.5E before decreasing gradually to 4.5 mmyr between 90.5E and 94E due to the crustal shortening across the Qaidam basin. Shear strain on the ATF is terminated in a horsetail structure at 95E where the strain is split into the motion along the Danghe Nanshan fault Yema River Daxue Shan fault and north Altyn Tagh fault. Our strain rate fields show fault planes are nearly vertical beneath the ATF and there are obvious changes in the strike of the deep shearing part of the fault beneath the Akato Tagh bend and Aksay bend. The Akato Tagh and Pingding Shan bends feature higher peak strain rates and narrower width of the interseismic straining zone at the surface compared to straight sections like the Xorkoli segment. We observe longwavelength uplift signals in the East Kunlun Shan range Altun Shan range Qaidam basin restraining bends along the ATF and the Qilian Shan Nan Shan thrust belt. We consider uplift of the latter is controlled by the thrust motion of the active faults within it as almost all shortening within it occurs across the fault zones. Uplift around restraining bends along the ATF exhibits a larger rate at their inside corners which is evidence of potential verticalaxis rotation within the bends. Our results provide a noteworthy example of how the strain is accumulated and terminated on a largescale intraplate strikeslip fault. | 2024-10-01T00:00:00Z | ['10.1016/j.epsl.2024.118919', '2024E&PSL.64418919W'] | ['Altyn Tagh fault', 'Qilian Shan – Nan Shan thrust belt', 'Strain accumulation', 'Slip Partitioning', 'Sentinel-1 InSAR', 'Restraining Bends'] | Deciphering interseismic strain accumulation and its termination on the centraleastern Altyn Tagh fault from highresolution velocity fields | 2,024 | 0 | 0.22 | ['PUB_HTML'] | 0 | null |
2024GCN.36765....1L | MASTERSAAO robotic telescope Global MASTERNet httpobserv.pereplet.ru Lipunov et al. 2010 Advances in Astronomy vol. 2010 30L located in South Africa South African Astronomical Observatory started inspect of the Fermi GRB 240625B Fermi GBM team GCN 36763 errorbox 17047 sec after notice time and 17076 sec after trigger time at 20240626 034311 UT with upper limit up to 18.2 mag. The observations began at zenith distance 80 deg. The sun altitude is 23.9 deg. The galactic latitude b 16 deg. longitude l 218 deg. Real time updated cover map and OT discovered available here httpsmaster.sai.msu.rusitemaster2observ.phpid2508418 We obtain a following upper limits. TmidT0 Date Time Site Coord J2000 Filt. Expt. Limit Comment 17107 20240626 034311 MASTERSAAO 05h 23m 38.92s 19d 41m 29.1s C 60 17.7 17265 20240626 034550 MASTERSAAO 05h 19m 55.38s 17d 48m 33.1s C 60 17.8 17424 20240626 034828 MASTERSAAO 05h 16m 41.27s 15d 55m 48.2s C 60 17.8 17582 20240626 035107 MASTERSAAO 05h 13m 53.84s 14d 01m 37.5s C 60 17.8 17741 20240626 035346 MASTERSAAO 05h 11m 24.01s 12d 06m 09.2s C 60 17.7 17902 20240626 035627 MASTERSAAO 05h 31m 21.76s 19d 42m 51.8s C 60 17.7 18060 20240626 035905 MASTERSAAO 05h 23m 43.61s 19d 41m 39.5s C 60 18.0 18302 20240626 040307 MASTERSAAO 05h 20m 03.20s 17d 48m 39.0s C 60 18.2 18461 20240626 040546 MASTERSAAO 05h 16m 48.76s 15d 55m 23.6s C 60 18.1 18620 20240626 040825 MASTERSAAO 05h 13m 54.54s 14d 01m 43.8s C 60 18.1 Filter C is a clear unfiltred band. The observation and reduction will continue. The message may be cited. | 2024-06-01T00:00:00Z | ['2024GCN.36765....1L'] | null | Fermi GRB 240625B Global MASTERNet observations report | 2,024 | 0 | 0.12 | ['PUB_HTML'] | 0 | null |
2016SPIE.9906E..40N | The W. M. Keck Observatory WMKO has a good track record at addressing large critical faults which impact observing. Our performance tracking and correcting chronic minor faults has been mixed yet this class of problems has a significant negative impact on scientific productivity and staff effectiveness. We have taken steps to address this shortcoming. This paper outlines the creation of a program to identify categorize and rank these chronic operational issues track them over time and develop management options for their resolution. The success of the program at identifying these chronic operational issues and the advantages of dedicating observatory resources to this endeavor are presented. | 2016-07-01T00:00:00Z | ['2016SPIE.9906E..40N', '10.1117/12.2233846'] | null | Addressing chronic operational issues at the W. M. Keck Observatory | 2,016 | 0 | 0.14 | ['PUB_HTML'] | 0 | null |
2016RoAJ...26...47S | Due to their pointlike aspect and to their lack of significant proper motion quasars represent the ideal objects for modeling quasiinertial directions in space. For that reason the present primary conventional reference frame the ICRF2 is constructed from the set of the celestial coordinates of 3414 extragalactic objects most of them being quasars. Thus each newly discovered quasar must be considered as a potential ideal astrometric marker. Therefore it looks interesting to compile in a regular basis all the recorded quasars at a given epoch. This constitutes the aim of the LQAC Large Quasar Astrometric Catalogue. We present here the third release of this catalog named as the LQAC3 insisting on the related strategy of compilation and on the various items it contains in the fields of astrometry redshift photometry morphology and magnitude. | 2016-01-01T00:00:00Z | ['2016RoAJ...26...47S'] | null | The large catalog of quasars and the LQAC3 compilation | 2,016 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2023tncm.confE...5S | As single stellar evolution cannot explain the existence of blue stragglers BSs several formation scenarios involving binaries have been put forward with mass transfer and direct collisions taking the lead. A third mechanism operating on its own or enhancing the former is the KozaiLidov mechanism where the amplitude of the inner binary in a hierarchical triple system changes via secular torque of its outer companion eventually leading to a merger of the inner binary and the formation of a BS.While much of our knowledge of the binarity of BSs comes from multiyear radial velocity campaigns e.g. WOCS these approaches are necessarily insensitive to the most distant binaries like those predicted by the KozaiLidov mechanism. These companions on wide orbits may be visible through direct highresolution imaging.We observed 51 BSs in 10 open clusters with the speckle interferometers Zorro and Alopeke at both Gemini telescopes reaching a spatial resolution of about 25 mas the diffraction limit at 500nm. Our observations probe for mainsequence companions down to a mass close to 0.3 Msun revealing that about 10 of BSs have these distant mainsequence companions. Ongoing spectroscopy will reveal whether the companions can be considered bound. | 2023-08-01T00:00:00Z | ['2023tncm.confE...5S', '10.5281/zenodo.8298474'] | ['Zenodo community notacrowd2023'] | Constraining a multiple stellar origin of blue stragglers via speckle imaging | 2,023 | 0 | 0.32 | ['PUB_HTML'] | 0 | null |
2023yCat..74900566J | In this work we have expanded on the efforts of Leisman et al. 2017ApJ...842..133L Cat. JApJ842133 and selecting two samples of HUDs restrictive and broad from SDSS and ALFALFA 100 per cent Haynes et al. 2018ApJ...861...49H Cat. JApJ86149 survey observations now with no environmental restriction included in the selection process. We also selected matched comparison samples for each HUDs sample based on their HI masses and distances to test for differences in the environmental preferences of HUDs. P We choose to follow Leisman et al. 2017ApJ...842..133L Cat. JApJ842133 in defining a restrictively selected sample HUDsR of 71 HIbearing ultradiffuse sources with halflight radii rSUBgeffSUBgt1.5kpc SUBg0SUBgt24magarcsecSUP2SUP and MSUBgSUBgt16.8mag and a more broadly selected sample HUDsB of 183 sources with rSUBreffSUBgt1.5kpc ltr rSUBeffSUBgtgt24magarcsecSUP2SUP and MSUBrSUBgt17.6 corresponding to the surface brightness and radius limits from van Dokkum et al. 2015ApJ...798L..45V and van der Burg Muzzin amp Hoekstra 2016AampA...590A..20V respectively with absolute magnitude limits as defined by Leisman et al. 2017ApJ...842..133L Cat. JApJ842133. Table A1 gives the observed quantities and optical properties of our sample. P 1 data file. | 2023-01-01T00:00:00Z | ['2023yCat..74900566J'] | ['Galaxies: photometry', 'H I data', 'Positional data', 'Optical'] | VizieR Online Data Catalog HIbearing ultradiffuse ALFALFA galaxies Janowiecki 2019 | 2,023 | 0 | 0.27 | null | 0 | null |
2023EGUGA..2510912N | Human technology is vulnerable to space weather a natural hazard. Highvoltage electric power transmission grids constitute one of the most critical manmade technological systems vulnerable to space weather driven geomagnetically induced currents GICs. In this study we perform an analysis of 1 measured GIC data collected at midlatitudes by U.S. power utilities during the period from 2010 to 2021 and 2 the corresponding geomagnetic field information for each event. The study includes a statistical analysis of all events and an overview of the top three highest GIC recordings in the data. We show that roughly 80 of the events are associated with the main phase of geomagnetic storms while about 20 are associated with sudden storm commencement. | 2023-05-01T00:00:00Z | ['10.5194/egusphere-egu23-10912', '2023EGUGA..2510912N'] | null | Analysis of geomagnetically induced currents over the continental United States | 2,023 | 0 | 0.06 | ['PUB_HTML', 'PUB_PDF'] | 0 | null |
2023yCat..36780145M | We present the galaxy groups and clusters based on the miniJPAS data and the AMICO algorithm Adaptive Matched Identifier of Clustered Objects. The miniJPAS data cover an area of 1 deg2 centered on the AEGIS field to the same depths with the same 54 narrow band plus 2 broader band nearUV and nearIR filters anticipated for the full JPAS survey. The cluster sample is accompanied by two other catalogues one listing the cluster members with probabilistic associations and listing the candidate clusters BGGs. P 3 data files. | 2023-07-01T00:00:00Z | ['2023yCat..36780145M'] | ['Clusters: galaxy', 'Surveys', 'Redshifts', 'X-ray sources', 'Optical'] | VizieR Online Data Catalog miniJPAS survey. clusters and galaxy groups Maturi 2023 | 2,023 | 0 | 0.27 | null | 0 | null |
2023yCat..36720027B | The complete dataset analyzed in the paper. Note compared to the whole MATLAS sample galaxies PGC058114 and PGC071531 were excluded. P 1 data file. | 2023-01-01T00:00:00Z | ['2023yCat..36720027B'] | ['Galaxy catalogs', 'Abundances', 'Morphology'] | VizieR Online Data Catalog Galaxies outside clusters Bilek 2023 | 2,023 | 0 | 0.23 | null | 0 | null |
2023spfi.confE..18M | Seismic constraints on stellar surface gravities have been instrumental in improving spectroscopic pipelines. On the other hand constraints on photospheric chemical abundances are a necessary ingredient to any inference about global stellar properties and to enable robust tests of stellar internal structures. In this contribution I will review the synergies between stellar spectroscopy and asteroseismology and discuss current limitations and future prospects in particular in the light of current and future spacephotometry missions such as PLATO and the ESA candidate M7 mission HAYDN. | 2023-09-01T00:00:00Z | ['2023spfi.confE..18M', '10.5281/zenodo.8334990'] | ['galactic archaeology', 'asteroseismology', 'haydn', 'Zenodo community spectralfidelity23'] | Spectral Fidelity and Asteroseismology | 2,023 | 0 | 0.3 | ['PUB_HTML'] | 0 | null |
2023yCat..36719002B | The catalogue of flybys in 118 debris disk systems is based on the Gaia eDR3 astrometric data and radial velocities. It includes the masses compiled from literature Stassun et al. 2019AJ....158..138S Cat. IV38 and the computed Hill radius. Using the Gaia eDR3 astrometric data and radial velocities of the sample as well as all the sources in a specific region of the sky we reconstructed the relative linear motions in the last 5Myr and made predictions for the next 2Myr. Relating the Hill radius of each debris disk system and the closest distances reached by the two sources we defined the flyby events in terms of position and time with uncertainties. P 2 data files. | 2023-02-01T00:00:00Z | ['2023yCat..36719002B', '10.26093/cds/vizier.36719002'] | ['YSOs', 'Stars: distances', 'Stars: masses'] | VizieR Online Data Catalog Flybys in debris disk systems with Gaia eDR3 Bertini 2023 | 2,023 | 0 | 0.2 | ['PUB_HTML'] | 0 | null |
2023pses.conf79943S | We present a study of atmospheric disturbances on Mars observed throughout Martian Year 36 from 7 February 2021 to 26 December 2022 using images taken by the cameras MARCIMars Reconnaissance Orbiter and VMCMars Express. The objective is to determine whether these disturbances waves cyclones dust storms global cloud development during the Aphelion Cloud Belt and others that evolve at different latitudes and longitudes leave their imprint on the meteorological detectors of the MEDA instrument on the Perseverance rover operating in Jezero crater. In particular we compare these observations with the surface pressure measurements made by MEDA throughout this period SnchezLavega et al. 2023. P SnchezLavega et al. Journal of Geophysical Research Planets 128 e2022JE007480 2023 httpsdoi.org10.10292022JE007480 | 2023-07-01T00:00:00Z | ['2023pses.conf79943S'] | ['Mars atmosphere', 'Mars images', 'Mars pressure'] | Atmospheric Disturbances in Martian Year 36 from Orbiters during the Operation of Rover Perverance | 2,023 | 0 | 0.27 | null | 0 | null |
2023yCatp061000205M | The W43MM1 ALMA observations were carried out between September 2014 and June 2015 project number 2013.1.01365.S using the 12m interferometric array. With baselines ranging from 13 to 1045m the 1.3mm image is sensitive to emission on angular scales from the synthesized beam 0.37x0.53 2400AU at 5.5kpc to the filtering scale of the interferometer for our observations 12. The W43MM1 cloud was imaged with a 33field mosaic covering its 2.1pcx1.4pc extent. The complete dataset contains eight spectral windows of which the one most used here is dedicated to the 1.3mm continuum centred at 233.45GHz with a bandwidth of 1.9GHz and a channel step of 977kHz. The complementary data taken with the 7m interferometric array were not used because of their low signaltonoise ratio. P 1 data file. | 2023-09-01T00:00:00Z | ['2023yCatp061000205M'] | ['Molecular clouds', 'Radio sources', 'Morphology'] | VizieR Online Data Catalog Cores detected at 1.3mm in W43MM1 Motte 2018 | 2,023 | 0 | 0.24 | null | 0 | null |
2023pses.conf79597D | Craters are typical features on the surface of planets. Their origin is diverse and comprises the impact of meteorites explosive volcanism sink holes etc all of them surface reshaping mechanisms that can be related in greater or lesser extent to the geodynamics of the bodies. Among the different processes high energy cratering often implies a notable modification of the magnetization state of the rocks which is recorded by their magnetic bearings. Later the evolution in the different atmospheres might also change the magnetic properties of the minerals 12. Therefore the magnetic investigations can be used to understand environmental features at the time when the event occurred as well as those that followed the formation event 3. On Earth volcanoes are continuously monitored both byremote sensing and insitu with parametric nets of sensors that permit their study along all their phases 4. There are also several techniques devoted to the identification and study of impact craters. However these techniques mostly the ones that imply in situ and multiparametric measurements are not feasible in the planetary exploration context. One would expect that the upcoming era of exploration of Mars and the Moon would permit the establishment of nets of stations by the study features as well as highresolution measurements with remote sensing platforms flying at low altitudes 10 100 m like helicopters 5 or balloons. This work presents the technology developed at INTA Space Magnetism Area and several studies performed in terrestrial analogues that mimic those expected in the planetary exploration context. Acknowledgements The field campaigns have been funded by the Spanish Government through the grants ESP201570184 R1 ESP201788930R PID2020119208RBI00 and RTI2018099615B100 the aerial platforms for magnetometry in MAGMA project with MAGMA NFQ Ventures. P 1 Lillis et al. 2010. J. Geophys. Res 115 E07007 P 2 Purucker M.E. amp Waaler K.A. 2013 Crustal magnetism. Vol. 5 Geomagnetism. M. Kono ed. Elsevier P 3 William W.J. et al. 2013. Gravity and magnetic exploration. Cambr. Univ. Press 502 p. 4 Hunt et al. 2013 Wiley. Online Library. DOI 10.1029RF003p0189 P 4 Fernndez J. et al. 2021 Sci Rep 11 2540. DOI 10.1038s41598021822923 P 5 Balaram B. et al. 2018 AIAA Atmospheric Flight Mechanics Conference. DOI10.25146.20180023 | 2023-07-01T00:00:00Z | ['2023pses.conf79597D'] | ['High-resolution magnetometry', 'magnetic instrumentation', 'magnetic anomalies', 'volcanoes', 'impact'] | Space Magnetism Activities for Planetary Exploration | 2,023 | 0 | 0.24 | null | 0 | null |
2023yCat..74915248W | We observed the PPPS target stars using the UCLES spectrograph Diego et al. 1990SPIE.1235..562D on the 3.9m AngloAustralian Telescope from 2009 February until 2015 January. UCLES achieved a resolution of 45000 with a 1arcsec slit and we aimed to achieve a signaltonoise ratio SN of 100 at 5500 per spectral pixel at each epoch resulting in exposure times ranging from 100 to 1200s. An iodine absorption cell provided wavelength calibration from 5000 to 6200. P Table A1 gives the complete set of final radial velocities from 105 PPPS targets. Table A2 summarizes the final dispositions of all PPPS targets e.g. published companion candidate or doublelined binary. P 3 data files. | 2023-02-01T00:00:00Z | ['2023yCat..74915248W'] | ['Exoplanets', 'Radial velocities', 'Spectra: optical'] | VizieR Online Data Catalog PanPacific Planet Search PPPS. VIII. Wittenmyer 2020 | 2,023 | 0 | 0.17 | null | 0 | null |
2023spfi.confE...1V | Separating stars enriched in the s and rprocesses of nucleosynthesis is usually done by analysing element ratios of mainly sprocess elements like Ba or La to mainly rprocess elements like Eu. The situation gets more complex when analysing CEMPrs stars which are CarbonEnriched MetalPoor objects enriched in a mixture of s and relements. These objects possibly resulting from the iprocess of nucleosynthesis are notoriously difficult to classify based on elemental ratio. Recent theoretical studies have outlined that the s i and rprocesses produce distinct isotopic mixtures. However isotopic abundances are notoriously difficult to measure from atomic lines because isotopic shifts of atomic lines are negligible compared to the line width. However in contrast with the spectral lines of even isotopes the lines of the odd isotopes are affected by hyperfine splitting HFS. It is thus possible to measure the odd fraction of the isotopic mixture fBaodd and to relate it to a given nucleosynthetic process either sprocess or irprocesses. In this talk some atomic isotopic diagnostics will be reviewed. Recent progress on how the isotopic mixture can constrain nucleosynthetic processes will be presented. The current limits on fBaodd determinations from highresolution spectra will be addressed. | 2023-09-01T00:00:00Z | ['2023spfi.confE...1V', '10.5281/zenodo.8341113'] | ['Zenodo community spectralfidelity23'] | Atomic isotopic ratio measurements | 2,023 | 0 | 0.29 | ['PUB_HTML'] | 0 | null |
2023yCat..19269008W | We observed WASP148 with the highresolution R110000 WIYNNEID spectrograph on 2021 April 26 and obtained 24 RV measurements with fixed 900s exposure times from UT 5071140. See Section 2.1.1. P We also obtained 38 RV measurements of WASP148 with continuous KeckHIRES observations from UT6141438 on 2021 June 9. All KeckHIRES observations were obtained with the C2 decker 14x0.861 R60000. During June 11 we also obtained a 45minute iodinefree HIRES template spectrum of WASP148 using the B3 decker 14.0x0.574 R72000. See Section 2.1.2. P To directly measure the transit midtime we took photometric observations of WASP148 using the 42inch Hall telescope and 1m Planewave telescope at Lowell Observatory the 1m Nickel telescope at Lick Observatory and an array of seven 4.5inch Unistellar eVscopes located in California and North Carolina while simultaneously observing the RM effect with KeckHIRES. The obtained light curves are provided in Figure 2. In addition to the simultaneous photometric observations our analysis also incorporates two photometric transits obtained with the 1.5m RitcheyChretien Telescope as well as TESS light curves derived from the MIT QuickLook Pipeline. Seven transits of WASP148b were observed in TESS Sectors 2426 from 2020 April 16 to July 04 with 30 minute exposures. See Section 2.2. P 2 data files. | 2023-11-01T00:00:00Z | ['2023yCat..19269008W'] | ['Spectra: optical', 'Radial velocities', 'Photometry', 'Exoplanets'] | VizieR Online Data Catalog Spectroscopic and transit obs. of WASP148 Wang 2022 | 2,023 | 0 | 0.32 | null | 0 | null |
2023yCatp052003701Z | The VRIc photometric observations of the field of the McNeils Nebula were carried out in the period from August 2004 to November 2021 with the 2m RitcheyChretienCoude RCC and the 5070cm Schmidt telescopes administered by the Rozhen National Astronomical Observatory Bulgaria and the 1.3m RitcheyChretien RC telescope administered by the Skinakas Observatory of the University of Crete Greece. Seven different CCD cameras were used to obtain the observations as follows VersArray 1300B and Andor iKonL BEX2DD on the 2m RCC telescope Photometrics CH360 and Andor DZ436BV on the 1.3m RC telescope and SBIG ST8 SBIG STL11000M and FLI PL16803 on the 5070cm Schmidt telescope. All frames were taken through a standard JohnsonCousins VRIc set of filters. Twilight flatfields in each filter were obtained every clear evening or morning. The frames acquired with the cameras on the 2m RCC and the 1.3m RC telescopes are biasframe subtracted and flatfield corrected. The frames obtained with the cameras on the 5070cm Schmidt telescope are darkframe subtracted and flatfield corrected. The photometric data were reduced using subroutine DAOPHOT in the IDL software package. As a reference sequence we used the VRIc comparisons reported in Semkov 2006IBVS.5683....1S. All data were analyzed using the same aperture which was chosen to have a 5arcsec radius and background annulus from 10arcsec to 15arcsec. The average value of the errors in the reported magnitudes is 0.010.02mag for the Ic and Rc band data and 0.010.03mag for the V band data. P 3 data files. | 2023-11-01T00:00:00Z | ['2023yCatp052003701Z'] | ['Stars: variable', 'Stars: pre-main sequence', 'Photometry: VRI'] | VizieR Online Data Catalog V2764 Ori and LkHa 301 longterm photometry Zidarova 2022 | 2,023 | 0 | 0.26 | null | 0 | null |
2023yCat..36820102P | CHEOPS photometry of WASP178 reduced with PIPE and detrended as described in the paper. P 1 data file. | 2023-09-01T00:00:00Z | ['2023yCat..36820102P'] | ['Stars: double and multiple', 'Exoplanets', 'Photometry', 'Optical'] | VizieR Online Data Catalog WASP178b CHEOPS light curves Pagano 2024 | 2,023 | 0 | 0.22 | null | 0 | null |
2023yCat..36670136V | The dataset analyzed in this work was taken from the ALMA Evolutionary study of High Mass Protocluster Formation in the Galaxy ALMAGAL survey 2019.1.00195.L PI S. Molinari that targeted over 1000 dense clumps with Mgt500MSUBSUB based on the Herschel HiGal survey P The derived column densities of all isotopologues are presented in Table B.1 for the reported excitation temperature. P 1 data file. | 2023-02-01T00:00:00Z | ['2023yCat..36670136V', '10.26093/cds/vizier.36670136'] | ['Masers', 'Interstellar medium', 'Millimetric/submm sources'] | VizieR Online Data Catalog Methanol deuteration in highmass protostars Van Gelder 2022 | 2,023 | 0 | 0.3 | ['PUB_HTML'] | 0 | null |
2017JDSO...13..165B | Data gathered from a 22Inch Newtonian AltAz telescope and a Celestron Micro Guide eyepiece were used to measure the double star STF 747AB. Students from Apple Valley High School determined the separation to be 39.97 arc sec and the position angle to be 227.91 degrees. The students also used data from the digitized sky survey and determined a separation of 39.99 arc sec and a position angle of 225 degrees. The research was semiindependent from the Vanguard Double Star Workshop 2016 in Apple Valley California. | 2017-04-01T00:00:00Z | ['2017JDSO...13..165B'] | null | Student Measurements of Double Star STF 747AB | 2,017 | 0 | 0.12 | null | 0 | null |
2017JDSO...13..140K | The LSPM catalog Lepine and Shara 2005 is a rich source for CPM pairs we thought already exhausted but as we found during research for our report A new concept for counterchecking of assumed CPM pairs Knapp and Nanson 2016 there are still many potential CPM pairs indicated in LSPM which as of the beginning of 2016 are not listed in the WDS catalog. A first part of about 40 such objects is presented here. | 2017-04-01T00:00:00Z | ['2017JDSO...13..140K'] | null | CPM Pairs from LSPM so far not WDS Listed | 2,017 | 0 | 0.06 | null | 0 | null |
2017JDSO...13...99K | Binary star HIP 4849 was observed on October 18 2013 UT using an EMCCD camera on the 2.1Meter telescope at Kitt Peak National Observatory. HIP 4849 had a separation rho of 0.725 and a position angle theta of 79.32. This observation did not deviate significantly from the predicted orbit. | 2017-01-01T00:00:00Z | ['2017JDSO...13...99K'] | null | Speckle Interferometry of Binary Star HIP 4849 | 2,017 | 0 | 0 | null | 0 | null |
2017JDSO...13...95M | We report on the measurement of position angle and separation of 93 binary pairs. The data was obtained using the NURO Telescope at the Anderson Mesa location of Lowell Observatory 20 miles east of Flagstaff Arizona on May and September 2012. We gathered the data using the 2K x 2K CCD cameraNASACAMat the prime focus of the 31 inch telescope. The data was transferred and analyzed at the Humacao University Observatory by undergraduate students undertaking research projects. | 2017-01-01T00:00:00Z | ['2017JDSO...13...95M'] | null | Observation Report for the Year 2012 Humacao University Observatory | 2,017 | 0 | 0 | null | 0 | null |
2015AGUFM.P11E..05W | The climate of Mars during the late Noachian 34 Ga remains a longstanding mystery. Over the last three decades the key debate has been whether the valley networks and other fluvial features were carved by rain in a warm wet Earthlike climate or by snowmelt in a mainly cold climate. Recently it has become clear that close intercomparison between the geology and 3D climate model predictions can be used to move this debate forward. Here I describe new work comparing threedimensional simulations under warm and cold climate scenarios with the surface distribution of valley networks. I discuss how the lack of periglacial landforms at equatorial latitudes the periglacial paradox and destabilizing climate influence of Tharsis can be used to rule out scenarios where the surface water inventory was extremely high indicating a mainly cold snowmeltdriven scenario for valley network formation is most likely. Finally I discuss plausible episodic warming mechanisms and the importance of early Mars to our conception of exoplanet habitability. | 2015-12-01T00:00:00Z | ['2015AGUFM.P11E..05W'] | ['5704 Atmospheres', 'PLANETARY SCIENCES: FLUID PLANETS', '6296 Extra-solar planets', 'PLANETARY SCIENCES: SOLAR SYSTEM OBJECTS', '5405 Atmospheres', 'PLANETARY SCIENCES: SOLID SURFACE PLANETS', '5455 Origin and evolution', 'PLANETARY SCIENCES: SOLID SURFACE PLANETS'] | Snow or rain on early Mars | 2,015 | 0 | 0.1 | null | 0 | null |
2017JGRA..12211481T | This study examines multipoint observations during a conjunction between Magnetospheric Multiscale MMS and Van Allen Probes on 7 April 2016 in which a series of energetic particle injections occurred. With complementary data from Time History of Events and Macroscale Interactions during Substorms Geotail and Los Alamos National Laboratory spacecraft in geosynchronous orbit 16 spacecraft in total we develop new insights on the nature of energetic particle injections associated with substorm activity. Despite this case involving only weak substorm activity maximum AE lt300 nT during quiet geomagnetic conditions in steady belowaverage solar wind a complex series of at least six different electron injections was observed throughout the system. Intriguingly only one corresponding ion injection was clearly observed. All ion and electron injections were observed at lt600 keV only. MMS reveals detailed substructure within the largest electron injection. A relationship between injected electrons with energy lt60 keV and enhanced whistler mode chorus wave activity is also established from Van Allen Probes and MMS. Drift mapping using a simplified magnetic field model provides estimates of the dispersionless injection boundary locations as a function of universal time magnetic local time and L shell. The analysis reveals that at least five electron injections which were localized in magnetic local time preceded a larger injection of both electrons and ions across nearly the entire nightside of the magnetosphere near geosynchronous orbit. The larger ion and electron injection did not penetrate to L lt 6.6 but several of the smaller electron injections penetrated to L lt 6.6. Due to the discrepancy between the number penetration depth and complexity of electron versus ion injections this event presents challenges to the current conceptual models of energetic particle injections. | 2017-11-01T00:00:00Z | ['10.1002/2017JA024554', '2017JGRA..12211481T'] | ['energetic particle injections', 'radiation belts', 'substorms', 'chorus waves', 'plasma sheet', 'inner magnetosphere'] | Multipoint Observations of Energetic Particle Injections and Substorm Activity During a Conjunction Between Magnetospheric Multiscale MMS and Van Allen Probes | 2,017 | 0 | 0.34 | ['PUB_HTML'] | 43 | null |
2017JGRA..12211373F | In this work observations of multispacecraft mission Time History of Events and Macroscale Interactions during Substorms are used for statistical investigation of dipolarization fronts in the nearEarth plasma sheet of the magnetotail. Using very stringent criteria 460 events are detected in almost 10 years of mission data. Minimum variance analysis is used to determine the normal directions of the phase fronts providing evidence for the existence of a natural symmetry of these phenomena given by the neutral sheet of the magnetotail. This finding enables the definition of a local coordinate system based on the Tsyganenko model reflecting the intrinsic orientation of the neutral sheet and therefore the dipolarization fronts. In this way the comparison of events with very different background conditions is improved. Through this study the statistical results of Liu Angelopoulos Runov et al. 2013 are both confirmed and extended. In a case study the knowledge of this plane of symmetry helps to explain the concave curvature of dipolarization fronts in the XZ plane through phase propagation speeds of magnetoacoustic waves. A second case study is presented to determine the central current system of a passing dipolarization front through a constellation of three spacecraft. With this information a statistical analysis of spacecraft observations above and below the neutral sheet is used to provide further evidence for the neutral sheet as the symmetry plane and the central current system. Furthermore it is shown that the signatures of dipolarization fronts are under certain conditions closely related to that of flux ropes indicating a possible relationship between these two transient phenomena. | 2017-11-01T00:00:00Z | ['2017JGRA..12211373F', '10.1002/2017JA024682'] | ['dipolarization fronts', 'minimum variance analysis', 'magnetotail', 'plasma sheet', 'THEMIS', 'neutral sheet'] | The Plasma Sheet as Natural Symmetry Plane for Dipolarization Fronts in the Earths Magnetotail | 2,017 | 0 | 0.14 | ['PUB_HTML'] | 2 | null |
2023yCat..74913606P | We expand a set of 25 blue compact dwarfs BCDs studied in Brorby et al. 2014MNRAS.441.2346B by selecting BCDs over all metallicities up to a distance of 60Mpc. Crossreferencing the BCD population defined by Izotov Thuan amp Stasinska 2007ApJ...662...15I Cat. JApJ66215 and the NED catalogue with the Chandra archive we find a total of 21 additional BCDs with Chandra observations GALEX observations and published metallicities. We add this to our sample for an overall sample size of 46 BCDs. P For the final sample we determine SFRs using GALEX UV data following the methods used in previous studies Brorby et al. 2014MNRAS.441.2346B and Brorby et al. 2016MNRAS.457.4081B. We obtain metallicities from published values all of them obtained through the directtemperature method with an exception. The distance and metallicity measurements from reported values in the literature are listed in Table A1. Xray source photometry information is listed in Table A2 and our UV and IR measurements and corresponding SFRs are detailed in Table A3. P 3 data files. | 2023-02-01T00:00:00Z | ['2023yCat..74913606P'] | ['Binaries: X-ray', 'Galaxies', 'X-ray sources', 'Abundances', 'Photometry: ultraviolet', 'Infrared'] | VizieR Online Data Catalog Effects of metallicity on HMXB formation Ponnada 2020 | 2,023 | 0 | 0.17 | null | 0 | null |
2023yCat..74930730M | All the data required for this study were taken from the literature. The nearIR fluxes were calculated from the magnitudes at respective wavelengths which were obtained from the 2MASS archive Cutri et al. 2003tmc..book.....C Cat. II246 archive. IRAS Neugebauer et al. 1984ApJ...278L...1N fluxes at 12 25 60 and 100m and WISE Wright et al. 2010AJ....140.1868W fluxes at 3.4 4.6 12 and 22m were used to span the mid and farIR emission. In addition we have used archived fluxes from Akari Ishihara et al. 2010AampA...514A...1I Cat. II297 at its 65 90 140 and 160m bands to trace the emission from cold dust down to 30K. The 2MASS and Akari data used for this study are available at the NASAIPAC Infrared Science Archive. P Our sample of WR PNe and welsPNe are from the catalogue of spectral classification of CSPNe given by Weidmann amp Gamen 2011AampA...526A...6W Cat. JAA526A6. We have taken the nebular H fluxes and electron densities from Stasinska amp Szczerba 1999AampA...352..297S Cat. JAA352297. Emissionline fluxes of OIII and HeII are obtained from StrasbourgESO Catalogue of Galactic PNe Acker et al. 1992ESOPN...1....1A Cat. V84. Distances to PNe in our sample are from Frew Parker amp Bojicic 2016MNRAS.455.1459F. P 3 data files. | 2023-03-01T00:00:00Z | ['2023yCat..74930730M'] | ['Planetary nebulae', 'Stars: Wolf-Rayet', 'Photometry: infrared'] | VizieR Online Data Catalog Infrared properties of planetary nebulae Muthumariappan 2020 | 2,023 | 0 | 0.25 | null | 0 | null |
2014AGUFMSM11B..05A | Understanding particle acceleration in the magnetotail during substorms requires knowledge of changes in the global magnetospheric configuration and the local fields and microinstabilities caused by processes associated with reconnection. To understand global structure of the magnetotail during substorms we use the UCLA global magnetohydrodynamic MHD simulation code and to understand local dynamics we couple the MHD simulation with the iPIC3D implicit particleincell code. The MHD code provides realistic initial and boundary conditions for the iPIC3D code which models the reconnection and evolution of the substorm dipolarization front DF selfconsistently with full kinetic physics. In the first case study we use a two dimensional version of iPIC3D to investigate the multiscale nature of the electron energization during a substorm on February 15 2008. In this multiscale simulation the electric and magnetic fields show the quadrupolar signature of HallMHD absent in the resistive MHD case. We note that during this event just like in the case of the MHD dipolarization fronts are formed mainly earthward of the neutral line. In the PIC simulation after a few seconds an active Xpoint forms and DFlike structures form about every two seconds and propagate earthward. The presence of the macroscopic scale magnetic field featuring a significant dipolar component nearer the Earth affects the reconnection process causing the production of multiple repeating DFs. The electrons are preferentially accelerated in the separatrices and reach energies of 100 keV or more. This acceleration of the plasma associated with the DFs is greater than that occurring near the Xpoint for this substorm. We have extended this study to three dimensions since it is known that DFs develop 3D structures. Compared to 2D simulations conducted in a meridian plane GSM XZ coordinates important additional aspects are present when the GSM Y coordinate is included e.g. the flapping and bending of the current layer the development of instabilities such as ballooning lower hybrid drift and interchange instabilities. | 2014-12-01T00:00:00Z | ['2014AGUFMSM11B..05A'] | ['2721 Field-aligned currents and current systems', 'MAGNETOSPHERIC PHYSICS', '2723 Magnetic reconnection', 'MAGNETOSPHERIC PHYSICS', '2744 Magnetotail', 'MAGNETOSPHERIC PHYSICS', '7863 Turbulence', 'SPACE PLASMA PHYSICS'] | Acceleration of Electrons in the Earths Magnetotail during Substorms Using MultiScale Simulations | 2,014 | 0 | 0 | null | 0 | null |
2023spfi.confE..24C | Nowadays there is a huge amount of valuable observing material available in public archives of highresolution spectrographs. The community can benefit from the reanalysis of these spectra to obtain precise parametrisation and chemical compositions of stars in particular by combining multiple observations of the same star. However to ensure consistency there is an important work of homogenisation of the spectra coming from different observational configurations or even different instruments. Common calibration and validation samples are also required. In this talk I will present my latest works where I have combined thousands of spectra from 1 different instruments to study a sample of open cluster stars and the Gaia FGK Benchmark stars. I will show which science we can do from such systematic queries to public spectral archives strategies to homogenise the analysis and how to evaluate the precision and accuracy. | 2023-09-01T00:00:00Z | ['2023spfi.confE..24C', '10.5281/zenodo.8328991'] | null | Using public archives of high resolution spectrographs | 2,023 | 0 | 0.31 | ['PUB_HTML'] | 0 | null |
2015EPSC...10..555B | Analyzing data from the ion sensor RPCICA flying on the european spacecraft Rosetta we study the dynamics of the interaction between the solar wind ions and a partially ionized atmosphere around a comet further than 2 AU away from the Sun. We give a close picture of this interaction with a first case study to then consider the whole low activity period through a statistical study and characterize the time evolution of this dynamics. | 2015-10-01T00:00:00Z | ['2015EPSC...10..555B'] | null | Mass loading of the solar wind near comet 67P at low activity | 2,015 | 0 | 0.06 | ['PUB_PDF'] | 0 | null |
2023yCat..36790018R | FITS file images of circumstellar disk in Ksband total intensity with VLTSPHEREIRDIS for HD 169142 and PDS 201. P FITS file images of circumstellar disk in Hband total intensity with VLTSPHEREIRDIS for HD 129590. P The stars are located at the mathematical centers of the arrays. P The units are in detector counts. P The SPHERE data were reduced with three different data reduction methods for reference differential imaging KarhunenLoeve Image Projection KLIP Data Imputation using KarhunenLoeve DIKL and Data Imputation using sequential Nonnegative Matrix Factorization DIsNMF. P 2 data files. | 2023-08-01T00:00:00Z | ['2023yCat..36790018R'] | ['Stars: early-type', 'Infrared'] | VizieR Online Data Catalog DIKL method for high contrast imaging Ren 2023 | 2,023 | 0 | 0.21 | null | 0 | null |
2023yCat..36720183A | Observables for 15062 stars deduced from Gaia DR3 data are presented. For each star the Gaia DR3 identification number is given as well as the spectral line broadening the projected surface rotation velocity the effective temperature the surface gravity the luminosity the dominant frequency of variability in the Gaia G band the amplitude of this dominant frequency the radius and the projected surface rotation frequency. The radius is computed from the luminosity and effective temperature. Missing values of the observables are indicated in the same format as measured values for coding convenience. P 2 data files. | 2023-02-01T00:00:00Z | ['2023yCat..36720183A', '10.26093/cds/vizier.36720183'] | ['Stars: dwarfs', 'Stars: variable', 'Stars: B-type', 'Stars: F-type', 'Effective temperatures', 'Rotational velocities'] | VizieR Online Data Catalog Gaia DR3 data of 15062 gravitymode pulsators Aerts 2023 | 2,023 | 0 | 0.27 | ['PUB_HTML'] | 0 | null |
2023yCat..18840107Z | In this paper we work with two sets of K2 light curves 1 the Campaign 1 C1 target sample from the K2 Galactic Archaeology Program GAP Stello 2015ApJ...809L...3S amp 2017 JApJ83583 which comprises 8630 stars and 2 all nonGAP C1 targets 13016 in total. Results from the Bayesian Asteroseismology data Modeling BAM for the former sample have been published in Stello 2017 JApJ83583. P We apply the BAM pipeline to 13016 C1 targets with VJ light curves not in the GAP sample. We identify 31 red giants that have detectable oscillation excesses. An additional 73 objects are potential giants. See Section 4. P 1 data file. | 2023-10-01T00:00:00Z | ['2023yCat..18840107Z'] | ['Stars: giant', 'Asteroseismology', 'Optical', 'Infrared sources', 'Models'] | VizieR Online Data Catalog The BAM pipeline applied to K2 LCs of red giants Zinn 2019 | 2,023 | 0 | 0.17 | null | 0 | null |
2023yCat..74941724J | We use the YJband spectra of 20 dwarfs 25 giants and 18 supergiants taken with WINERED. They were observed with the WIDEmode giving the resolution of around 28000. The spectra between 0.91 and 1.35m are covered with 20 echelle orders from 42nd to 61st. The observations were carried out with the 1.3m Araki Telescope at Koyama Observatory Kyoto Sangyo University in Japan from July 2015 to May 2016. A part of the spectra of giants and supergiants were used in Matsunaga et al. 2020ApJS..246...10M to identify absorption lines of neutroncapture elements. P 6 data files. | 2023-05-01T00:00:00Z | ['2023yCat..74941724J'] | ['Stars: dwarfs', 'Stars: giant', 'Stars: supergiant', 'Effective temperatures', 'Abundances: [Fe/H]', 'Spectra: infrared'] | VizieR Online Data Catalog Effect of surface gravity on linedepth ratios Jian 2020 | 2,023 | 0 | 0.23 | null | 0 | null |
2023yCat..74941237S | In Prudil amp Skarka 2017MNRAS.466.2602P Cat. JMNRAS4662602 we found 3341 stars to show the Blazhko effect based on the look of the frequency spectra and the presence of the equidistant side peaks with amplitudes above SNRgt3.5. This sample was studied again employing automatic procedures and applying subsequent visual inspection of all the frequency spectra of the studied stars to discard the stars with ambiguous modulation. Since we are now interested in the characteristics of the Blazhko effect we performed additional data examination and analysis. P 1 data file. | 2023-05-01T00:00:00Z | ['2023yCat..74941237S'] | ['Stars: variable', 'Milky Way', 'Photometry', 'Optical'] | VizieR Online Data Catalog Blazhko effect in Galactic RR Lyrae II Skarka 2020 | 2,023 | 0 | 0.23 | null | 0 | null |
2023ursi.confE..81K | Frame based decomposition of fields provides a rigorous flexible and effective tool to represent planar source field distributions as summations of Gaussian windows. The field radiated by each window can be approximated as a Gaussian beam in its paraxial region. In this context beam shooting and bouncing techniques have been proposed as an alternative to corresponding ray methods for describing wave propagation in complex environments. ComplexSource beams which are closely related to Gaussian beams provide rigorous solutions for several canonical problems. The objective of this paper is to investigate relations between Gaussian beams radiated by frame windows and ComplexSource beams. Such an approach would open the door to extending the applicability of frame decomposition methods enhancing Gaussian beam shooting by means of solutions provided by ComplexSource beams. | 2023-10-01T00:00:00Z | ['10.23919/URSIGASS57860.2023.10265369', '2023ursi.confE..81K'] | ['Propagation'] | ComplexSource Beam Representation of the Fields Radiated by a Gaussian Window | 2,023 | 0 | 0.06 | ['PUB_HTML'] | 1 | null |
2023ursi.confE..62Y | The shooting and bouncing ray SBR method is a general and efficient estimation method for calculating the radar scattering crosssection of complex targets of electric universities. In this paper the SBR method is used to analyze the distortion of the farfield directional map of the electric large platform antenna and the farfield magnitude at each target observation angle is obtained by invoking the raytracking modules ray magnitude tracking and ray phase tracking for calculation then the antenna farfield is quickly calculated by collecting the field strength contribution of the rays at each target observation angle. This method overcomes the problem that needs to consume huge memory and computation time and avoids the calculation frequency changes due to the algorithm and requires recalculation. The method was compared with a Cassegrain antenna excited by an 18 GHz horn antenna and it was concluded that SBR greatly improved the computational efficiency of the antenna far field. | 2023-10-01T00:00:00Z | ['10.23919/URSIGASS57860.2023.10265514', '2023ursi.confE..62Y'] | ['Time-frequency analysis; Target tracking; Horn antennas; Memory management; Prediction methods; Directive antennas; Ray tracing'] | An Antenna Farfield Prediction Method Based on Shooting and Bouncing Ray Method | 2,023 | 0 | 0.24 | ['PUB_HTML'] | 0 | null |
2023yCat..18750142X | Our sample consists of 129 red giant branch stars in the Galactic bulge and they have already been minutely discussed by Zoccali 2008 JAA486177 and Johnson 2014 JAJ14867. P The observations were carried out at the VLTUT2 with the FLAMESGIRAFFE spectrograph at a resolution power 20000. The original program by Zoccali 2008 JAA486177 contained four fields but as the HR11 spanning 55905835 was the only setup including measurable copper lines only two bulge fields 5.253.02 and 012 were observed in the HR11 HR13 and HR15 setups ESO3 Program 073.B0074. P Johnson 2014 JAJ14867 analyzed 156 giants with the final signaltonoise ratio SN of each coadded spectrum exceeding 70 and without strong TiO absorption bands. As the spectral SNs were rather low for some stars the final sample utilized here only included 129 objects. P 1 data file. | 2023-10-01T00:00:00Z | ['2023yCat..18750142X'] | ['Stars: giant', 'Abundances', 'Spectra: optical'] | VizieR Online Data Catalog Copper abundances of Galactic bulge red giant stars Xu 2019 | 2,023 | 0 | 0.17 | null | 0 | null |
2023yCat..75025668V | The superoutbursts of most SU UMa stars show a pronounced quasiperiodicity occurring rather regularly one linear ephemeris with a standard deviation of only 510 per cent of the corresponding period Vogt 1980AampA....88...66V. This property allows the determination of a rough value of the cycle length even if only a few superoutbursts are recorded. In the present study we are limited to those dwarf novae for which no reliable cycle length values are published in the latest online version of the catalogue of Ritter amp Kolb 2003AampA...404..301R Cat. Bcb. The main sources were light curves determined by AAVSO members available in the LCG data base of that organization as well in the photometric All Sky Automated Survey ASAS Pojmanski 2002AcA....52..397P Cat. II264 catalogue and in the Catalina Sky Survey CSS Drake et al. 2009ApJ...696..870D Cat. JApJ696870. For a few cases this information was complemented from ASASSN Kochanek et al. 2017PASP..129j4502K and Gaia alerts Gaia Collaboration et al. 2018AampA...616A...1G Cat. I345. P 4 data files. | 2023-11-01T00:00:00Z | ['2023yCat..75025668V'] | ['Stars: variable', 'Stars: dwarfs', 'Novae', 'Binaries: cataclysmic', 'Optical'] | VizieR Online Data Catalog Superoutburst of 206 SU UMatype dwarf novae Vogt 2021 | 2,023 | 0 | 0.27 | null | 0 | null |
2016JPhCS.718e2038S | EAS array of novel type have been constructed on the base of ARGOYBJ experiment Tibet China. It consists of the four specially designed scintillator endetectors capable to measure two main EAS components hadrons through thermal neutrons n and electrons e. The results of simulation for these arrays using CORSIKA and GEANT4 codes are presented. Simulated thermal neutron and electron lateral distributions are compared with experimental data. Obtained distributions are compared with those obtained by other arrays. | 2016-05-01T00:00:00Z | ['10.1088/1742-6596/718/5/052038', '2016JPhCS.718e2038S'] | null | Electron and thermal neutron lateral distribution functions in EAS at high altitude | 2,016 | 0 | 0.1 | ['PUB_HTML'] | 1 | null |
2023yCat..75030292K | We presented a new photometric analysis of the core of R136 using the second epoch data from VLTSPHERE instrument in the nearIR. We observed R136 in H and K filters in better atmospheric observing conditions and longer exposure time than the first epoch. This enabled us to detect twice as many sources in H and K as we have detected in the first epoch in J and K in the FOV of IRDIS 10.8x12.1 covering almost 2.7x3.0pc of R136 core. Among 1658 and 2528 detected sources in H and K respectively we found 1499 common sources between these two sets of data where 76 per cent of these sources have visual companion closer than 0.2 which is higher than the value found in the first epoch in 2015 data Khorrami et al. 2017AampA...602A..56K Cat. JAA602A56. About 71 per cent of the newly detected sources are located in the outer region rgt3 of the cluster. P 3 data files. | 2023-11-01T00:00:00Z | ['2023yCat..75030292K'] | ['Clusters: open', 'Photometry: infrared'] | VizieR Online Data Catalog NIR photometry of the core of R136 Khorrami 2021 | 2,023 | 0 | 0.24 | null | 0 | null |
2023yCat..75024074M | In order to determine the kinematic model parameters and calibrate the MSUBVSUBFeH and PLZ relations in the KSUBsSUB and WSUB1SUB bands using the statisticalparallax method with better precision we need a large sample of RRLs with 1 known periods and pulsation modes 2 accurate and precise apparent mean magnitude in the Johnson V 2MASS KSUBsSUB and WISE WSUB1SUB passbands 3 proper motions metallicities radial velocities and extinctions in one of the passbands. Initially our sample for this work consists of 850 RRLs. Depending on the spectroscopic data source we subdivide this sample of RRLs into two parts the first one is the most complete sample of Galactic field RRL type variables employed in our previous statisticalparallax analysis Dambis et al. 2013MNRAS.435.3206D Cat. JMNRAS4353206 this list initially includes a total of 403 Galactic field RRL stars but one RRL is discarded due to current updates the second part consists of 448 RRL type variables which have our own new spectroscopic data acquired as a result of observations performed with SALT telescope. P 1 data file. | 2023-10-01T00:00:00Z | ['2023yCat..75024074M'] | ['Stars: variable', 'Milky Way', 'Parallaxes: trigonometric', 'Abundances: [Fe/H]', 'Proper motions', 'Radial velocities', 'Optical', 'Infrared'] | VizieR Online Data Catalog Periodluminositymetallicity relation of RRLs Muhie 2021 | 2,023 | 0 | 0.26 | null | 0 | null |
2023yCat..75015309H | We have compiled a photometric catalogue of stars in the Kepler field utilizing photometry from Gaia Stromgren and 2MASS catalogues. We created a metallicity calibration based on APOGEE spectroscopy to obtain a metallicity for our photometric sample and then performed welldefined colour and magnitude cuts to ensure our data set was a representative sample of the underlying population of stars. We then derived temperatures and angular diameters using the IFRM which were then used to derive stellar radii and stellar mass through Bayesian isochrone fitting. The resultant parameters were compared favourably with previous results from the literature especially giving stellar radii with relative uncertainties around 3.4 per cent. Planetary radii uncertainties of 6.2 per cent hence indicate a major uncertainty contribution from the Kepler planet to star ratio. P 1 data file. | 2023-10-01T00:00:00Z | ['2023yCat..75015309H'] | ['Exoplanets', 'Stars: double and multiple', 'Effective temperatures', 'Abundances: [Fe/H]', 'Stars: masses', 'Stars: diameters', 'Optical'] | VizieR Online Data Catalog Confirming known planetary trends with Kepler Hansen 2021 | 2,023 | 0 | 0.23 | null | 0 | null |
2016JPhCS.718b2014M | Following the discovery of neutrino oscillations by the SuperKamiokande collaboration recently awarded with the Nobel Prize two generations of long baseline experiments had been setup to further study neutrino oscillations. The first generation experiments K2K in Japan Minos in the States and Opera in Europe focused in confirming the SuperKamiokande result improving the precision with which oscillation parameters had been measured and demonstrating the SUBSUB appearance process. P Second generation experiments T2K in Japan and very recently NOA in the States went further being optimized to look for genuine three neutrino phenomena like nonzero values of SUB13SUB and first glimpses to leptonic CP violation LCPV and neutrino mass ordering NMO. P The discovery of leptonic CP violation will require third generation setups at the moment two strong proposals are ongoing Dune in the States and HyperKamiokande in Japan. This review will focus a little more in these future initiatives. | 2016-05-01T00:00:00Z | ['2016JPhCS.718b2014M', '10.1088/1742-6596/718/2/022014'] | null | Long Baseline Neutrino Experiments | 2,016 | 0 | 0.1 | ['PUB_HTML'] | 1 | null |
2023ursi.confE...6P | The paper deals with deterministicstochastic modeling of the current diffusion equation CDE. Deterministic part of the analysis is carried out by means of standard finite element method FEM. Stochastic postprocessing of the deterministic results is carried out by means of nonintrusive stochastic collocation method SCM and analysis of variance ANOVA approach. Some numerical results illustrating the convergence of SCM confidence interval and sensitivity indices are given in the paper. | 2023-10-01T00:00:00Z | ['2023ursi.confE...6P', '10.23919/URSIGASS57860.2023.10265345'] | ['Plasma confinement; Sensitivity; Stochastic processes; Mathematical models; Numerical models; Finite element analysis; Analysis of variance'] | DeterministicStochastic Modeling of Current Diffusion Equation CDE for Plasma Confinement | 2,023 | 0 | 0.17 | ['PUB_HTML'] | 0 | null |
2016MPLA...3150022F | Incorporating the generalized uncertainty principle GUP into the tunneling mechanism we have studied the tunneling radiation of the scalar particles and fermions from the fivedimensional SchwarzschildTangherlini black hole. The results showed that the GUP corrected temperatures do not only depend on the mass of ST black hole but are also affected by the gravity effects correction . Besides the slows down the Hawking temperature increasing and causes the existence of remnants in black hole evaporation. | 2016-01-01T00:00:00Z | ['2016MPLA...3150022F', '10.1142/S021773231650022X'] | ['The generalized uncertainty principle', 'the five-dimensional black hole', 'GUP corrected Hawking temperature', '04.62.+v', '04.70.Dy', 'Quantum field theory in curved spacetime', 'Quantum aspects of black holes evaporation thermodynamics'] | Modified tunneling radiation of the scalar particles and Dirac particles from a fivedimensional black hole | 2,016 | 0 | 0.1 | ['PUB_HTML', 'PUB_PDF'] | 2 | null |
2016MPLA...3150116D | Nonminimally coupled scalar field cosmology has been studied in this work within the framework of Einstein gravity. In the background of homogeneous and isotropic FriedmannLemaitreRobertsonWalker FLRW spacetime nonminimally coupled scalar field having selfinteracting potential is taken as the source of the matter content. The constraint of imposing Noether symmetry on the Lagrangian of the system not only determines the infinitesimal generator the symmetry vector but also the coupling function and the selfinteracting potential for the scalar field. By choosing appropriately a point transformation in the augmented space one of the transformed variables is cyclic for the Lagrangian. Finally using constants of motion the solutions are analyzed. | 2016-06-01T00:00:00Z | ['2016MPLA...3150116D', '10.1142/S0217732316501169'] | ['Non-minimal coupling', 'scalar field', 'Noether symmetry', '04.20.Cv', 'Fundamental problems and general formalism'] | A study of dynamical equations for nonminimally coupled scalar field using Noether symmetric approach | 2,016 | 0 | 0.16 | ['PUB_HTML', 'PUB_PDF'] | 4 | null |
2016MPLA...3150007N | We calculate finite temperature corrections to the energy of the Casimir effect of a two conducting parallel plates in a general weak gravitational field. After solving the KleinGordon equation inside the apparatus mode frequencies inside the apparatus are obtained in terms of the parameters of the weak background. Using Matsubaras approach to quantum statistical mechanics gravityinduced thermal corrections of the energy density are obtained. Wellknown weak static and stationary gravitational fields are analyzed and it is found that in the low temperature limit the energy of the system increases compared to that in the zero temperature case. | 2016-12-01T00:00:00Z | ['10.1142/S0217732316500073', '2016MPLA...3150007N'] | ['Casimir effect', 'gravitational field', 'finite temperature', '98.80.Bp', '98.80.Cq', 'Origin and formation of the Universe', 'Particle-theory and field-theory models of the early Universe'] | Thermal corrections to the Casimir energy in a general weak gravitational field | 2,016 | 0 | 0.12 | ['PUB_HTML', 'PUB_PDF'] | 2 | null |
2023yCat..19270012P | For the photometric observations we used the 1.3m Devasthal Fast Optical Telescope DFOT and the 1.04m Sampurnanand Telescope ST operated by the Aryabhatta Research Institute of Observational Sciences ARIES. Table 2 shows the observation log of DFOT and ST photometric observations spanning 2018Oct to 2021Mar. P We also used the photometric observations by the Transiting Exoplanet Survey Satellite TESS. TESS was launched in 2018. The TESS data are publicly available at the the Barbara A. Mikulski Archive for Space Telescopes MAST portal. P The photometric data from other surveys were also used for period analysis but most of the times of minima TOMs were derived from SuperWASP Wide Angle Search for Planets data. The SuperWASP project is an ultrawideangle photometric survey observing the northern and southern hemispheres of the sky from the sites of La Palma Canary Islands and South African Astronomical Observatory Sutherland. Each site covers almost a 500degSUP2SUP part of the sky with the help of eight cameras. The SuperWASP public archive contains time series data of almost 18 million targets. P 2 data files. | 2023-11-01T00:00:00Z | ['2023yCat..19270012P'] | ['Binaries: eclipsing', 'Photometry', 'Optical'] | VizieR Online Data Catalog Longterm photometric analysis of 5 EBs Panchal 2022 | 2,023 | 0 | 0.16 | null | 0 | null |
2023yCat..36720031O | Radial velocities of all components and details about spectra of the triple star Delta Ori HR 1852 HD 36486 HIP 25930 ADS 4134 from the coude focus of the Ondrejov 2m reflector and the ELODIE and FEROS echele spectrographs in the blue region. The RVs of all three components were determined during the spectral disentangling threestep method in KOREL. P 2 data files. | 2023-01-01T00:00:00Z | ['2023yCat..36720031O'] | ['Binaries: eclipsing', 'Stars: O', 'Radial velocities'] | VizieR Online Data Catalog Triple star delta Ori radial velocities Oplistilova 2023 | 2,023 | 0 | 0.22 | null | 0 | null |
2016cosp...41E1041K | Phobos Sample Return is a mission currently studied by the European Space Agency ESA in collaboration with Russia. The main scientific goal is to return about 100 g of sample from the Martian moon Phobos. The current ESA Phase A study has identified a feasible mission with a launch in Sep 2024. It would arrive at Mars in Aug 2025 land on Phobos in April 2026 escape from Mars in September 2026 and bring back a sample to Earth in the summer of 2027. The spacecraft consists of a Propulsion Module PM a Lander Module LM an Earth Return Vehicle ERV and an Earth Reentry Capsule ERC. A sampling Acquisition Transfer and Containment system SATCS composed of a robotic arm sampling and sealing mechanism is responsible for the surface sampling operations. The PM is responsible for bringing the whole SC composite into Mars orbit. The LanderERVERC composite would separate from the PM after Mars Orbit Insertion. After a phase of 1 month spent observing Deimos from a quasisatellite orbit the composite would be transferred to Phobos vicinity for an extensive phase of detailed surface characterization which would allow the selection of the candidate landing site. The SC would then land on Phobos and remain on the surface for a few weeks. After some initial characterization of the surroundings the sample would be taken and transferred to the ERC. The ERV with the ERC would leave Phobos and return to Earth the LM would continue performing surface science on Phobos until several weeks after ERV departure. Shortly before atmospheric entry the ERC would separate from the ERV to enter the atmosphere safely. After recovery the sample would be returned into an analysis lab. This presentation will give the latest status of the mission study and outline future activities. | 2016-07-01T00:00:00Z | ['2016cosp...41E1041K'] | null | Phobos Sample Return a mission to return a sample from a Martian moon | 2,016 | 0 | 0.14 | null | 0 | null |
2017JGRA..12210157P | For the first time we have studied the rich internal structure of a magnetosheath highspeed jet. Measurements by the Magnetospheric Multiscale MMS spacecraft reveal largeamplitude density temperature and magnetic field variations inside the jet. The propagation velocity and normal direction of planar magnetic field structures i.e. current sheets and waves are investigated via fourspacecraft timing. We find structures to mainly convect with the jet plasma. There are indications of the presence of a tangential discontinuity. At other times there are small crossstructure flows. Where this is the case current sheets and waves overtake the plasma in the jets core region ahead and behind that core region along the jets path current sheets are overtaken by the plasma that is they move in opposite direction to the jet in the plasma rest frame. Jet structures are found to be mainly thermal and magnetic pressure balance structures notwithstanding that the dynamic pressure dominates by far. Although the jet is supermagnetosonic in the Earths frame of reference it is submagnetosonic with respect to the plasma ahead. Consequently we find no fast shock. Instead we find some evidence for a series of jets pushing ambient plasma out of their way thereby stirring the magnetosheath and causing anomalous sunward flows in the subsolar magnetosheath. Furthermore we find that jets modify the magnetic field in the magnetosheath aligning it with their propagation direction. | 2017-10-01T00:00:00Z | ['2017JGRA..12210157P', '10.1002/2017JA024471'] | ['magnetosheath', 'jet', 'structure', 'flow', 'discontinuity'] | Magnetosheath HighSpeed Jets Internal Structure and Interaction With Ambient Plasma | 2,017 | 0 | 0.29 | ['PUB_HTML'] | 25 | null |
2016cosp...41E..62A | Optically selected clusters from the CFHTLS and Xray selected clusters from the intersecting XXL Survey are compared. We first compare the properties of the 100 galaxy clusters common to both catalogues in the redshift range of 0.1 lt z lt 1.2. Then we focus on the properties of the missed clusters on both sides and stress the impact of AGN contamination in this comparison. Finally scaling relations involving optical and Xray quantities will be presented. | 2016-07-01T00:00:00Z | ['2016cosp...41E..62A'] | null | Comparison of Xray and optically selected galaxy clusters in the XXLN field | 2,016 | 0 | 0.06 | null | 0 | null |
2016cosp...41E1138L | We consider effects of cosmic rays CR and some other space phenomena on the Earths climate change. It is well known that the system of internal and external factors formatting the Earths climate is very unstable decreasing of planetary average annual temperature leads to an increase of planetary snow surface and decreasing of the total annual solar energy input into the system decreases the planetary temperature even more. And inverse increasing planetary temperature leads to an decrease of snow surface and increasing of the total solar energy input into the system increases the planetary temperature even more. From this follows that even energetically small factors acted long time in one direction may have a big influence on climate change. In our opinion the most important of these factors are CR mostly through its influence on planetary cloudiness and space dust SD through their influence on the flux of solar irradiation and on formation of clouds these actions are in one direction. It is important that CR and SD influenced on global climate change in the same direction. Increasing of CR planetary intensity leads to increasing of formation clouds especially low clouds on altitudes smaller than 3 km increasing annual average of raining and decreasing of annual average planetary temperature. Increasing of SD decreases of solar irradiation and increases cloudiness what leads also to decreasing of annual average planetary temperature. Moreover interactions of CR particles with dust granules decreases their dimensions what increased effectiveness of their actions on clouds. We consider data great variations of planetary temperature much before the beginning of the Earths technological civilization mostly caused by moving of the solar system around our Galaxy centre and collisions with moleculardust clouds. We consider in details not only situation during the last hundred years but also situation in the last one thousand years and especially situation during Maunder minimum of solar activity during many thousand and many millions years. It is shown that very big changes in climate were caused also by some rarely phenomena as impacts of asteroids and nearby supernova explosions with great influence on biosphere. We discuss also the problem on forecasting of global climate change what is especially important for saving present civilization from great climate catastrophes. | 2016-07-01T00:00:00Z | ['2016cosp...41E1138L'] | null | Cosmic rays and other rpace phenomena influenced on the Earths climate | 2,016 | 0 | 0.24 | null | 0 | null |
2017ARep...61..342V | The homogenization of inhomogeneities in the elemental composition of the interstellar medium due to stellar evolution and weak mixing are inevitably related to the action of shocks. This paper considers the influence of variations in the elemental composition on the thermal and ionizational evolution of a collisional gas with the solar metallicity that is cooled behind a shock front with a velocity of 50120 kms. The intensities of lines of heavy elements in plasma cooling behind a shock front depend not only on variations in the elemental composition but also on the shock velocity due to the different values of the critical density for the transition to the equilibrium level populations in atoms and ions of heavy elements. This circumstance can be used to determine the elemental composition of cool and warm gas of the interstellar medium as well as the thermal history of the gas. | 2017-04-01T00:00:00Z | ['2017ARep...61..342V', '10.1134/S1063772917040175'] | null | The influence of variations of the elemental composition on the thermal properties of gas behind shock fronts | 2,017 | 0 | 0.19 | ['PUB_HTML'] | 2 | null |
2017ATel10591....1S | We obtained optical spectra of ASASSN17it ATel 10555 and ASASSN17jl AT 2017foy on UT 2017 July 22.4 with the Goodman Spectrograph on the SOAR telescope. | 2017-07-01T00:00:00Z | ['2017ATel.10591...1S', '2017ATel10591....1S'] | ['Supernovae', 'Transient'] | Spectroscopic Classification of ASASSN17it and ASASSN17jl as Type Ia SNe | 2,017 | 0 | 0.06 | ['PUB_HTML'] | 0 | null |
2017ATel10690....1L | The SwiftBAT detected an increase in hard Xray emission 1550 keV coming from the ultracompact Xray binary 4U 1543624 around 2017 August 9. The MAXI daily monitoring also shows a gradual increase in 2.020.0 keV Xray intensity as of 2017 August 19. SwiftXRT ToO monitoring of the source was triggered and shows an increase in unabsorbed flux to 1.06E9 ergscm2s in the 0.310.0 keV energy band as of 2017 August 26. ATCA performed ToO observations for approximately 4 hours in the 5.5 GHz and 9.0 GHz bands while the antennas were in the 1.5A array configuration from 11251609 UTC on 2017 August 23. The source was not detected in either band. | 2017-08-01T00:00:00Z | ['2017ATel.10690...1L', '2017ATel10690....1L'] | ['Binary', 'Black Hole', 'Neutron Star'] | SwiftBAT Detects Increase in Hard Xray Emission from the Ultracompact Xray Binary 4U 1543624 | 2,017 | 0 | 0.17 | ['PUB_HTML'] | 0 | null |
2017ATel10096....1N | PESSTO the Public ESO Spectroscopic Survey for Transient Objects see Smartt et al. 2015 A amp A 579 40 httpwww.pessto.org reports the following supernova classification. | 2017-02-01T00:00:00Z | ['2017ATel10096....1N', '2017ATel.10096...1N'] | ['Supernovae', 'Transient'] | PESSTO spectroscopic classification of optical transients | 2,017 | 0 | 0 | ['PUB_HTML'] | 0 | null |
2017ATel10841....1K | ePESSTO the extended Public ESO Spectroscopic Survey for Transient Objects see Smartt et al. 2015 A amp A 579 40 httpwww.pessto.org reports the following supernova classifications. | 2017-10-01T00:00:00Z | ['2017ATel10841....1K'] | ['Supernovae'] | ePESSTO spectroscopic classification of optical transients | 2,017 | 0 | 0 | ['PUB_HTML'] | 0 | null |
2017AIPC.1815d0005K | When determining the phase from the projected fringes by using continuous wavelet transform CWT selection of wavelet is an important step. A new wavelet for phase retrieval from the fringe pattern with the spatial carrier frequency in the x direction is presented. As a mother wavelet zero order generalized Morse wavelet GMW is chosen because of the flexible spatial and frequency localization property and it is exactly analytic. In this study GMW method is explained and numerical simulations are carried out to show the validity of this technique for finding the phase distributions. Results for the Morlet and Paul wavelets are compared with the results of GMW analysis. | 2017-02-01T00:00:00Z | ['2017AIPC.1815d0005K', '10.1063/1.4976374'] | null | Optical phase distribution evaluation by using zero order Generalized Morse Wavelet | 2,017 | 0 | 0.1 | ['PUB_HTML'] | 1 | null |
2017AAS...22914102K | With the success of LISA Pathfinder the measurement of gravitational waves in space has taken an important step forward. We conduct an analysis of the measurement abilities of distinctive LISA detector designs examining how the lowfrequency bandedge behavior of the detector sensitivity curve affects measurement capabilities. We are particularly interested in LISAs ability to measure massive black holes that are merging near the bandedge with masses in the range of sim 1061010Modot. We examine the ringdown and insprial detectability over a wide range of Massive Black Hole MBH binaries along with a broad palette of possible LISA design parameters. | 2017-01-01T00:00:00Z | ['2017AAS...22914102K'] | null | Exploring Parameter Space Coverage of Various LISA Configurations | 2,017 | 0 | 0.06 | null | 0 | null |
2017AAS...22914610N | Future direct imaging mission concepts such as HabEx and LUVOIR aim to directly image and characterize Earthanalogs around nearby stars. With the scope and expense of these missions the exoplanet yield is strongly dependent on the frequency of Earthlike planets and the a priori knowledge of which stars specifically host suitable planetary systems. Groundbased radial velocity surveys can potentially perform the preselection of direct imaging missions at a fraction of the cost of a blind direct imaging survey. We present a simulation of such a survey. We consider both the WIYN and Large Binocular Telescope including weather conditions and limitations in telescope time fitted with spectrometers of varying sensitivities including iLocator and NEID. We recover simulated planets and their orbital parameters estimating the effectiveness of a precursor radial velocity survey. | 2017-01-01T00:00:00Z | ['2017AAS...22914610N'] | null | Simulating a Radial Velocity Precurser Survey for Target Yield Optimization for a Future Direct Imaging Mission | 2,017 | 0 | 0.17 | null | 0 | null |
2017A&A...607A..19P | Context. Dust impact into granular materials leads to crater formation and material ejection. BR Aims The impact of dust aggregates composed of a number NSUBpSUB of grains into a granular bed consisting of the same grains is studied as a function of impact velocity v and projectile size NSUBpSUB. No gravitational effects are included. BR Methods Granularmechanics simulations are used to study the outcome of dustaggregate impacts. The granular bed and the aggregates are composed of silica grains and have filling factor 0.36. BR Results Both the crater volume and the ejection yield increase sublinearly with total impact energy. No crater rims are formed. Crater shapes change from hemispheric to elongated when increasing either projectile size or velocity. The crater walls are compacted by the impact within a zone of a size comparable to the crater radius. Ejecta are produced at the edges of the impact only a small fraction of the ejecta stem from the projectile. The energy distribution of the ejecta follows at high energies a 1ESUP2SUP decay reminiscent of sputtering from atomic targets. The maximum of the distribution is shifted to higher energies for larger projectiles this is caused by the increasing depth from which ejected grains originate. BR Conclusions Due to the dissipative nature of intergranular collisions and the porosity of the target crater morphology and ejecta yield deviate characteristically from impacts into atomic materials. | 2017-10-01T00:00:00Z | ['2017A&A...607A..19P', '10.1051/0004-6361/201730954'] | ['planets and satellites: formation', 'protoplanetary disks', 'methods: numerical'] | Dustaggregate impact into granular matter A systematic study of the influence of projectile velocity and size on crater formation and grain ejection | 2,017 | 0 | 0.27 | ['PUB_HTML', 'PUB_PDF'] | 11 | null |
2017CBET.4449....2W | The available astrometry including a prediscovery observation from the 1.8m PanSTARRS1 telescope at Haleakala on Sept. 11.56 UT when the magnitude was measured to be 19.3 the following nearly parabolic orbital elements by G. V. Williams from 128 observations spanning Sept. 11Oct. 27 and an ephemeris appear on MPEC 2017U238. Epoch 2018 July 21.0 TT T 2018 July 19.1413 TT Peri. 246.8875 e 0.999295 Node 230.0961 2000.0 q 0.825409 AU Incl. 88.1012 | 2017-10-01T00:00:00Z | ['2017CBET.4449....2W'] | null | Comet C2017 T3 Atlas | 2,017 | 0 | 0.1 | ['PUB_HTML'] | 0 | null |
2017ATel10089....1D | On 2017 February 2 Swift resumed its daily Xray monitoring campaign of the Galactic center using the XRT Degenaar et al. 2015 JHEA 7 137 see link below. | 2017-02-01T00:00:00Z | ['2017ATel.10089...1D', '2017ATel10089....1D'] | ['Binary', 'Black Hole', 'Neutron Star', 'Transient'] | Swift resumes Xray monitoring observations of the Galactic center in 2017 | 2,017 | 0 | 0.14 | ['PUB_HTML'] | 0 | null |
2017AAS...22910203S | The MASSES Mass Assembly of Stellar Systems and their Evolution with the SMA survey a Submillimeter Array SMA largescale program is mapping molecular lines and continuum emission about the 75 known Class 0I sources in the Perseus Molecular Cloud. In this talk I present some of the key results of this project with a focus on the CO21 maps of the molecular outflows. In particular I investigate how protostars inherit their rotation axes from largescale magnetic fields and filamentary structure. | 2017-01-01T00:00:00Z | ['2017AAS...22910203S'] | null | Interferometric Mapping of Perseus Outflows with MASSES | 2,017 | 0 | 0.12 | null | 0 | null |
2017AAS...22914606S | The principal difficulty with detecting planets via direct imaging is that the target signal is similar in magnitude or fainter than the noise sources in the image. To compensate for this several methods exist to subtract the PSF of the host star and other confounding noise sources. One of the most effective methods is KarhunenLove Image Processing KLIP. The core algorithm within KLIP is Principal Component Analysis which is a member of a class of algorithms called Blind Source Separation BSS.We examine three other BSS algorithms that may potentially also be used for PSF subtraction Independent Component Analysis Stationary Subspace Analysis and Common Spatial Pattern Filtering. The underlying principles of each of the algorithms is discussed as well as the processing steps needed to achieve PSF subtraction. The algorithms are examined both as primary PSF subtraction techniques as well as additional postprocessing steps used with KLIP.These algorithms have been used on data from the Gemini Planet Imager analyzing images of Pic b. To build a reference library both Angular Differential Imaging and Spectral Differential Imaging were used. To compare to KLIP three major metrics are examined computation time signaltonoise ratio and astrometric and photometric biases in different image regimes e.g. speckledominated compared to Poissonnoise dominated. Preliminary results indicate that these BSS algorithms improve performance when used as an enhancement for KLIP and that they can achieve similar SNR when used as the primary method of PSF subtraction. | 2017-01-01T00:00:00Z | ['2017AAS...22914606S'] | null | Blind Source Separation Algorithms for PSF Subtraction from Direct Imaging | 2,017 | 0 | 0.16 | null | 0 | null |
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