source
stringlengths 1
2.05k
⌀ | target
stringlengths 1
11.7k
|
|---|---|
For the configuration where Uranus Neptune start out in a 6:5 MMR, also of the integrations were successful, but none of the solutions exhibited ice giant encounters with both gas giants. | For the configuration where Uranus Neptune start out in a 6:5 MMR, also of the integrations were successful, but none of the solutions exhibited ice giant encounters with both gas giants. |
In the subset of initial conditions where Saturn Uranus are in a 4:3 MMR, the configurations with Uranus Neptune in à 3:2 MMR and a 4:3 MMR can serve as good candidates for solar system formation, but the configuration with Uranus Neptune in a 5:4 MMR consistently leads to ejections. | In the subset of initial conditions where Saturn Uranus are in a 4:3 MMR, the configurations with Uranus Neptune in a 3:2 MMR and a 4:3 MMR can serve as good candidates for solar system formation, but the configuration with Uranus Neptune in a 5:4 MMR consistently leads to ejections. |
of the integrations with Uranus Neptune initially in a 3:2 MMR were successful, all of them exhibiting scattering with both ice giants. | of the integrations with Uranus Neptune initially in a 3:2 MMR were successful, all of them exhibiting scattering with both ice giants. |
In the context of the configuration with Uranus Neptune initially in a 4:3 MMR, of the integrations were successful, while of them lead to encounters of an ice giant with both gas giants. | In the context of the configuration with Uranus Neptune initially in a 4:3 MMR, of the integrations were successful, while of them lead to encounters of an ice giant with both gas giants. |
Examples of successful evolutions that start from the initial conditions described above are presented in figures (4) - (7), with final orbital parameters entered into table (2). | Examples of successful evolutions that start from the initial conditions described above are presented in figures (4) - (7), with final orbital parameters entered into table (2). |
Note that the scattering event in the evolution of the configuration where Saturn Uranus are initially in a 3:2 MMR and Uranus Neptune are in a 5:4 MMR (fig. | Note that the scattering event in the evolution of the configuration where Saturn Uranus are initially in a 3:2 MMR and Uranus Neptune are in a 5:4 MMR (fig. |
4) is considerably more violent than that in most other examples. | 4) is considerably more violent than that in most other examples. |
This is because majority of close encounters here is between Jupiter and Uranus, while in most other simulations, Saturn is responsible for scattering. | This is because majority of close encounters here is between Jupiter and Uranus, while in most other simulations, Saturn is responsible for scattering. |
It is important to understand that this is not a unique feature of the particular initial condition. | It is important to understand that this is not a unique feature of the particular initial condition. |
We have observed similar phenomena in simulations of other setups as well. | We have observed similar phenomena in simulations of other setups as well. |
Note that in a scenario where Jupiter and Saturn start out in a 5:3 MMR, the instability is brought on by their crossing of the 2:1 MMR, just as in the classical Nice model. | Note that in a scenario where Jupiter and Saturn start out in a 5:3 MMR, the instability is brought on by their crossing of the 2:1 MMR, just as in the classical Nice model. |
Much effort has been put into fine-tuning the classical Nice model’s initial conditions (Tsiaganis et al. | Much effort has been put into fine-tuning the classical Nice model's initial conditions (Tsiaganis et al. |
2005, Morbidelli et al. | 2005, Morbidelli et al. |
2005, Gomes et al. | 2005, Gomes et al. |
2005, Levison et al. | 2005, Levison et al. |
2008). |
|
What matters most, however, are the locations of the 2008).planets when Jupiter and Saturn are crossing the 2:1 MMR. | What matters most, however, are the locations of the planets when Jupiter and Saturn are crossing the 2:1 MMR. |
Let us now examine if the classical Nice model is compatible with any multi-resonant initial conditions from this family. | Let us now examine if the classical Nice model is compatible with any multi-resonant initial conditions from this family. |
We begin our calculation by measuring the semi-major axes of the four planets at the Jupiter/Saturn 2:1 MMR crossing in figure (2a) of Levison et al. ( | We begin our calculation by measuring the semi-major axes of the four planets at the Jupiter/Saturn 2:1 MMR crossing in figure (2a) of Levison et al. ( |
2008). | 2008). |
The values are listed in the second column of Table (3). | The values are listed in the second column of Table (3). |
Between encounters with MMR’s, migrations of Jupiter and Saturn are mostly due to scattering of planetesimals. | Between encounters with MMR's, migrations of Jupiter and Saturn are mostly due to scattering of planetesimals. |
Malhotra (1995) showed from conservation of angular momentum that this process obeys a relation, which upon integration can be written as where f is an empirically determined “efficiency,” listed in Table (3), and m, is the total scattered mass. | Malhotra (1995) showed from conservation of angular momentum that this process obeys a relation, which upon integration can be written as where $f$ is an empirically determined “efficiency," listed in Table (3), and $m_{s}$ is the total scattered mass. |
When applied to Jupiter and Saturn simultaneously, this relation can be used to “backtrace” the system’s migration, by roughly estimating the starting semi-major axes of Jupiter and the scattered mass m,. | When applied to Jupiter and Saturn simultaneously, this relation can be used to “backtrace" the system's migration, by roughly estimating the starting semi-major axes of Jupiter and the scattered mass $m_{s}$ . |
Setting Δας=(5/3)?/2ai,—(2)?/3a!, and Aa;=αὖ—a, with al,=5.45 AU yields a total scattered mass of 37mq and =5.69 AU. | Setting $\Delta a_S = (5/3)^{2/3} a_J^i - (2)^{2/3} a_J^f$ and $\Delta a_J = a_J^f - a_J^i$ with $a_J^f = 5.45$ AU yields a total scattered mass of $37 m_{\oplus}$ and $a_J^i = 5.69$ AU. |
a’,Neglecting high-order resonant encounters, we then use the calculated scattered mass and apply equation (4) to Uranus and Neptune todetermine their original | Neglecting high-order resonant encounters, we then use the calculated scattered mass and apply equation (4) to Uranus and Neptune todetermine their original |
more crowded regions. | more crowded regions. |
Iu this paper we present the results of a new search for variable stars iu NCC 1166 aud use the RR Lyrae in NGC 1166 to confirm the distance modulus and Oosterhoff classification of the cluster. | In this paper we present the results of a new search for variable stars in NGC 1466 and use the RR Lyrae in NGC 1466 to confirm the distance modulus and Oosterhoff classification of the cluster. |
We also prescut Fourier fits to the light curves aud derive physical properties for the stars from these fits. | We also present Fourier fits to the light curves and derive physical properties for the stars from these fits. |
A total of LO V aud 37 DB nuages of NGC L166 were obtained using the SOT imager ou the SOAR 1- un telescope in February aud December of 2008. | A total of $40$ $V$ and $37$ $B$ images of NGC 1466 were obtained using the SOI imager on the SOAR $4$ -m telescope in February and December of 2008. |
Au additional 15 V. aud. 13 DB images were obtained usine ANDICAAT on the SMARTS Τι telescope operated w the SMARTS from September 2006. to January 2007. | An additional $45$ $V$ and $43$ $B$ images were obtained using ANDICAM on the SMARTS $1.3$ -m telescope operated by the SMARTS from September 2006 to January 2007. |
This represents a larger data set than the 35 DV pairs obtained by Walker (1992).. | This represents a larger data set than the 35 BV pairs obtained by \citet{wa92b}. . |
Exposure times or the SOAR observations were between 30s and 300s or V aud between 60s aud 300s for D. but were usually 120s and 180s for the V. aud D observations. respectively, | Exposure times for the SOAR observations were between $30$ s and $300$ s for $V$ and between $60$ s and $300$ s for $B$, but were usually $120$ s and $180$ s for the $V$ and $B$ observations, respectively. |
SMARTS exposures were 1508 for cach filter. | SMARTS exposures were $450$ s for each filter. |
The images frou both telescopes were bias subtracted and flat-field corrected usingIRAF*. | The images from both telescopes were bias subtracted and flat-field corrected using. |
. As noted iu Walker (1992).. NGC 1166 is located near two very bright stars which create problems with scattered light across some of the images. especially iu many of the images obtained with the SATARTS telescope. | As noted in \citet{wa92b}, NGC 1466 is located near two very bright stars which create problems with scattered light across some of the images, especially in many of the images obtained with the SMARTS telescope. |
We used. the procedure described in detail by Stetson&Tarris(1988). to remove this scattered light: this was the same method cuploved by Walker(1992).. | We used the procedure described in detail by \citet{sh88} to remove this scattered light; this was the same method employed by \citet{wa92b}. |
Peter Stetsou's Daophot IL/Allstar packages (StetsonLOST.1992.1991) were used to locate. measure. and subtract stars from all images: this produced images that ouly contained the sky background and scattered light. | Peter Stetson's Daophot II/Allstar packages \citep{st87,st92,st94} were used to locate, measure, and subtract stars from all images; this produced images that only contained the sky background and scattered light. |
The subtracted images were then snoothed using a LosLO pixel median filter. | The subtracted images were then smoothed using a $40$ $40$ pixel median filter. |
The average sky level in the simoothecd nuages was determined aud then the smoothed nuages were subtracted from the original images. removing the backeround light. | The average sky level in the smoothed images was determined and then the smoothed images were subtracted from the original images, removing the background light. |
The average sky values were then added back into the new nuages. creating a final set of iniages with a coustaut sky backerouud. | The average sky values were then added back into the new images, creating a final set of images with a constant sky background. |
Stetson'*s Daophot ΠΑγίας packages were run ou the new set of nüages in to order obtain iustruieutal maenitudes for cach star. | Stetson's Daophot II/Allstar packages were run on the new set of images in to order obtain instrumental magnitudes for each star. |
Observations of the Laudolt standard fields PCG0231.. RULI9. SÀ95. aud SÁ9S Landolt1902) were used to determine an initial transformation from instrumental magnitudes to the standard system. | Observations of the Landolt standard fields PG0231, RU149, SA95, and SA98 \citep{la92} were used to determine an initial transformation from instrumental magnitudes to the standard system. |
Jolusouetal.(1999) showed Walkers plotometiv to be iu good agreement with USTΛΕΡΟΣ observations of NGC 1166. after these observations were transformed from the on-board UST system to the standard Jolusou-Cousius system. | \citet{jj99} showed Walker's photometry to be in good agreement with HST/WFPC2 observations of NGC 1466, after these observations were transformed from the on-board HST system to the standard Johnson-Cousins system. |
We compared the results of our initial transformation to the standard svsteni using Walkers photometry of isolated non-variable stars across a rauge of brightuesses within the cluster. | We compared the results of our initial transformation to the standard system using Walker's photometry of isolated non-variable stars across a range of brightnesses within the cluster. |
We made small corrections to the zero points aud color terms from our initial transformation equations iu order to achieve better agreement with Walkers photometrzy. | We made small corrections to the zero points and color terms from our initial transformation equations in order to achieve better agreement with Walker's photometry. |
This produced au average difference between our data and Walkers of AV=0.012£0.01 aud AB=0.026£0.02. | This produced an average difference between our data and Walker's of $ \Delta V = 0.012\pm0.01$ and $\Delta B =0.026\pm0.02$. |
This is a simular level of scatter to that obtained by (1999) iu their comparison with Walker. | This is a similar level of scatter to that obtained by \citet{jj99} in their comparison with Walker. |
The profile fitting photometry used in Daophot Il/Allstar does not work well in very crowded regions. such as the ceuter of NGC 1166. | The profile fitting photometry used in Daophot II/Allstar does not work well in very crowded regions, such as the center of NGC 1466. |
In order to locate variable stars in this region. the SOAR data on the cluster center was also searched using the ISISv2.2 inaese subtraction program (Alard20003. | In order to locate variable stars in this region, the SOAR data on the cluster center was also searched using the ISISv2.2 image subtraction program \citep{ca00}. |
. The original iniages were used for the ISIS processing as the scattered light is less of a problem when using inaee subtraction techniques. | The original images were used for the ISIS processing as the scattered light is less of a problem when using image subtraction techniques. |
The light curves produced by ISIS are in relative fluxes. | The light curves produced by ISIS are in relative fluxes. |
There is a iuethod to trausform the relative fluxes obtained by ISIS into maeuituces iu the standard system by using Daophot to obtain maguitudes of the stars in the reference frame created ly ISIS (Mochejskaetal.2001). | There is a method to transform the relative fluxes obtained by ISIS into magnitudes in the standard system by using Daophot to obtain magnitudes of the stars in the reference frame created by ISIS \citep{mo01}. |
. Four of our variable stars were coud ouly by ISIS (V31. V51. V51. V60). | Four of our variable stars were found only by ISIS $31$, $51$, $54$, $60$ ). |
These stars are ocated deep in the cluster center and are too crowded ο obtain accurate profile fitting photometry. even in the reference nuage. | These stars are located deep in the cluster center and are too crowded to obtain accurate profile fitting photometry, even in the reference image. |
These four light curves are shown in relative fluxes: for the other variables we preseut their ieht curves obtained from Daophot I/Allstar. | These four light curves are shown in relative fluxes; for the other variables we present their light curves obtained from Daophot II/Allstar. |
Figure d shows our CMD for NGC L166. | Figure \ref{cmd} shows our CMD for NGC 1466. |
The cluster features a well-defined horizontal brauch (ID) that extends across the instability strip. | The cluster features a well-defined horizontal branch (HB) that extends across the instability strip. |
The majority of the IID stars are blue. with few IID stars located redward of he instability strip. | The majority of the HB stars are blue, with few HB stars located redward of the instability strip. |
As was noted by Walker(1992).. the RR Lyrae stars appear to be less Iuninous than the blue ID stars near the blue οσο of the instability strip. | As was noted by \citet{wa92b}, the RR Lyrae stars appear to be less luminous than the blue HB stars near the blue edge of the instability strip. |
As can be seen in the feure. there are some non-variable stars in the instability strip region. | As can be seen in the figure, there are some non-variable stars in the instability strip region. |
These are duc to either poor photometry due to blending iu the cluster center or are line-of-sight field stars. | These are due to either poor photometry due to blending in the cluster center or are line-of-sight field stars. |
We used the V-band time series. which had more phase points than the B-band one. to identity candidate variable stars using Peter Stetsons Allfraine/Trial package (Stetson—1991). | We used the $V$ -band time series, which had more phase points than the $B$ -band one, to identify candidate variable stars using Peter Stetson's Allframe/Trial package \citep{st94}. |
. Period— searches ou the candidate variables were carried out using Supersmoother (ReimannL99L).. Dreger 2005).. aud a discrete Fourier transform (Ferraz-Mello1981) as implemented iu the Peranuso software suite?. | Period searches on the candidate variables were carried out using Supersmoother \citep{re94}, \citep{le04}, and a discrete Fourier transform \citep{ferraz81} as implemented in the Peranso software . |
. This produced light curves which were thon examuned by eve to coufirm the reality of each variable star candidate. | This produced light curves which were then examined by eye to confirm the reality of each variable star candidate. |
Light curves of potential RR Lyrac stars were then fit to template Leht curves (Lavdenu/1998) aud checked by eve in order to confirma variable classification and period. | Light curves of potential RR Lyrae stars were then fit to template light curves \citep{ly98} and checked by eye in order to confirm variable classification and period. |
Resulting primary periods are typically good to ΕΕΟΟΘΟΙ or 0.00002 days while errors for the secondary periods of RRd stars are slightly worse but on the same order of magnitude. | Resulting primary periods are typically good to $\pm 0.00001$ or $0.00002$ days while errors for the secondary periods of RRd stars are slightly worse but on the same order of magnitude. |
A similar search of the Πο curves produced with ISIS was done to find additional variables. | A similar search of the light curves produced with ISIS was done to find additional variables. |
Atotal of 62 variables were found. including 19 RR Lyracs. 1 additional candidate RR Lyrae. 2 loue- variables.a candidate anomalous Ceplicid. aud 9 variables of unknown classification. | Atotal of $62$ variables were found, including $49$ RR Lyraes, $1$ additional candidate RR Lyrae, $2$ long-period variables,a candidate anomalous Cepheid, and $9$ variables of unknown classification. |
We were able for the first time to identify double-mode (RBRd) variables none the RR Lyrae population of NCC Ll66, | We were able for the first time to identify double-mode (RRd) variables among the RR Lyrae population of NGC 1466. |
Of the | Of the |
two files. | two files. |
Radio nebulae with optical counterparts were transferred. to the optical file. | Radio nebulae with optical counterparts were transferred to the optical file. |
We also used information of optical nebulae among radio cetections by Caswell Tavnes (1987). | We also used information of optical nebulae among radio detections by Caswell Haynes (1987). |
The resulting input lists of optical and radio nebulae contain respectively 991 and 276 objects iu the present Milkv Way sector. whose directions were mspected. | The resulting input lists of optical and radio nebulae contain respectively 991 and 276 objects in the present Milky Way sector, whose directions were inspected. |
The whole Milkv. Way radio aud optical uebula catalogue currently has 1451 entries after cross-ijchtifications. and will be provided in a forthcoming study. | The whole Milky Way radio and optical nebula catalogue currently has 4454 entries after cross-identifications, and will be provided in a forthcoming study. |
It follows similar procedures as those used iu the construction of the dark nebula catalogue (Dutra Bica 2002) which has 5001 eutries. | It follows similar procedures as those used in the construction of the dark nebula catalogue (Dutra Bica 2002) which has 5004 entries. |
The results of the cluster survey will be available as Tables 3 and d in eletronic form at CDS (Strasbourg) via anouvimous ftp to edsarc.u-strasbe.fr. (130.79.128.5). respectively for optical aud radio nebulae. | The results of the cluster survey will be available as Tables 3 and 4 in eletronic form at CDS (Strasbourg) via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5), respectively for optical and radio nebulae. |
By cohunus: (1) running number: (2) aud (3) Galactic coordinates. CL) and (5) J2000.0 equatorial coordinates. (6) and (7) major aud minor augular dinieusious. (8) related nebulae. (9) class. (10) remarks inchiding distance R (in case | By columns: (1) running number; (2) and (3) Galactic coordinates, (4) and (5) J2000.0 equatorial coordinates, (6) and (7) major and minor angular dimensions, (8) related nebulae, (9) class, (10) remarks including distance $R$ (in case |
eracdicut along the ring (the dotted line in Fie. | gradient along the ring (the dotted line in Fig. |
7 shows linear fit of the data). | 7 shows linear fit of the data). |
Interestingly. the direction of this eracdient coincides with the direction of the main body rotation (Fig. | Interestingly, the direction of this gradient coincides with the direction of the main body rotation (Fig. |
5). | 5). |
Aloug P.A.=27° we observe the rise of the Πα ratio from 0.70.8 in the nucleus to ~1.5 a |eodS μι | Along $^{\rm o}$ we observe the rise of the $\alpha$ ratio from 0.7–0.8 in the nucleus to $\sim$ 1.3 at $\mid r \mid =
3''-4''$ . |
Similar increases in the Πα ratio iive been observed recently in a nuniber of edee-on spirals. e.g... UGC 10013 (Alatthews de (ης 2001 and references therein) | Similar increases in the $\alpha$ ratio have been observed recently in a number of edge-on spirals, e.g., UGC 10043 (Matthews de Grijs 2004 and references therein). |
Shock-heating due to starburst-driven wind is the usual explanation of such liue ratios. | Shock-heating due to starburst-driven wind is the usual explanation of such line ratios. |
Iu the case of ANI 1931-563 we uced additional spectral observations to confirm the presence of a large-scale wind. | In the case of AM 1934-563 we need additional spectral observations to confirm the presence of a large-scale wind. |
It is iuterestiug to note that two other PRCs with vouus or forming vines are classified as “superwind” ealaxies — NCC 660 (Armus et al. | It is interesting to note that two other PRGs with young or forming rings are classified as ”superwind” galaxies – NGC 660 (Armus et al. |
1990) and NGC 6286 (Shalvapina et al. | 1990) and NGC 6286 (Shalyapina et al. |
2001). | 2004). |
Possible polaraiug related spiral UGC 10013 also shows the presence of a large-scale wind (Matthews de Caijs 2001). | Possible polar-ring related spiral UGC 10043 also shows the presence of a large-scale wind (Matthews de Grijs 2004). |
One can propose that nuclear stirburst aud. correspondingly. starburst-divenu wind exteudius up to the outer kinematically decoupled structure are the natural consequences of an external accretion event. as suggested by uunucerical models (BCO3. and the model iu this paper). | One can propose that nuclear starburst and, correspondingly, starburst-driven wind extending up to the outer kinematically decoupled structure are the natural consequences of an external accretion event, as suggested by numerical models (BC03, and the model in this paper). |
A systematic shift in radial velocities derived from Πα aud [NITI| lines is evideut in Fig. | A systematic shift in radial velocities derived from $\alpha$ and [NII] lines is evident in Fig. |
7. | 7. |
It is not an unique feature siuce may spirals show the same behavior (e.g. Afanasiey et al. | It is not an unique feature since many spirals show the same behavior (e.g., Afanasiev et al. |
2001. Moiscey 2002). | 2001, Moiseev 2002). |
The difference in observed velocities may be explained dy the simple asstuuption that the [NIT| cussion line originates partially in shocks. due to a wind or a bar CAfanasiev et al. | The difference in observed velocities may be explained by the simple assumption that the [NII] emission line originates partially in shocks, due to a wind or a bar (Afanasiev et al. |
2001). | 2001). |
Both companion galaxies are giant spirals. | Both companion galaxies are giant spirals. |
The NW ealaxv (PCC 100092) demonstrates asviumetric. slightly nreenlar morphology without pronounced spiral aruis. | The NW galaxy (PGC 400092) demonstrates asymmetric, slightly irregular morphology without pronounced spiral arms. |
Subsets and Splits
No community queries yet
The top public SQL queries from the community will appear here once available.