source
stringlengths 1
2.05k
⌀ | target
stringlengths 1
11.7k
|
|---|---|
Àt one point in the simulation when the SAL is in a particularly shallow region the very large radiative losses produce a downllowing plume that is able {ο traverse (he entire vertical extent of (he computational domain. | At one point in the simulation when the SAL is in a particularly shallow region the very large radiative losses produce a downflowing plume that is able to traverse the entire vertical extent of the computational domain. |
This is shown clearly in a visualisation of the convecting plumes in Procvon given al ieicic.astro.ale.edu/inarjf To illustrate the response of the SAL to the turbulent overturning granules we plot the superachabaticily al 5 instants in Fis.4.. | This is shown clearly in a visualisation of the convecting plumes in Procyon given at $ www.astro.yale.edu/marjf $ To illustrate the response of the SAL to the turbulent overturning granules we plot the superadiabaticity at 5 instants in \ref{sal_procyon}. |
The photosphere. defined by the location at which the horizontally and temporally averaged temperature equals the effective temperature of ihe ID Procvon stellar model. is marked by a solid vertical line. | The photosphere, defined by the location at which the horizontally and temporally averaged temperature equals the effective temperature of the 1D Procyon stellar model, is marked by a solid vertical line. |
The solid horizontal line shows where the superacliabaticily is zero. | The solid horizontal line shows where the superadiabaticity is zero. |
Each plot is separated by 2.5 minutes in (ime. | Each plot is separated by 2.5 minutes in time. |
The time /0 is chosen as the time after which the svstem has reached. statistical thermal equilibrium. | The time $t0$ is chosen as the time after which the system has reached statistical thermal equilibrium. |
The ligure shows that over the quasi-periodic evele the SAL varies both in position and height. | The figure shows that over the 'quasi-periodic' cycle the SAL varies both in position and height. |
During part of the evele the outer region of the SAL lies above the photosphere. | During part of the cycle the outer region of the SAL lies above the photosphere. |
Li. Z.. Wang. Q. D.. and IIuneed. ο. 2007. MNRAS O'Sullivan. E.. Forbes. D. Α.. and Ponman. T. J. 2001. AINRAS Owen. R. A. and Warwick. BR. S. 2009. AINRAS Alannuecci. F. et al. | Li, Z., Wang, Q. D., and Hameed, S. 2007, MNRAS O'Sullivan, E., Forbes, D. A., and Ponman, T. J. 2001, MNRAS Owen, R. A. and Warwick, R. S. 2009, MNRAS Mannucci, F. et al. |
2005. AA Alareoni. A. and Hunt. L. IX. 2003. ApJ MeGaugh. S. S. et al. | 2005, A Marconi, A. and Hunt, L. K. 2003, ApJ McGaugh, S. S. et al. |
2010. ApJ Alulchaev. J. ον, and Jeltema. T. E. 2010. ApJ Navarro. J. F. 1998. preprint Pedersen. IX. et al. | 2010, ApJ Mulchaey, J. S., and Jeltema, T. E. 2010, ApJ Navarro, J. F. 1998, preprint Pedersen, K. et al. |
2006. New Astron. | 2006, New Astron. |
Rasmussen. J. et al. | Rasmussen, J. et al. |
2009. ApJ Read. A. M. and Ponman. T. J. 1998. MNRAS Revnivisey. M. et al. | 2009, ApJ Read, A. M. and Ponman, T. J. 1998, MNRAS Revnivtsev, M. et al. |
2008. | 2008. |
AGAA Roberts. T. P. and Warwick. BR. ο, 2000. AINRAS Robertson. D. et al. | A Roberts, T. P. and Warwick, R. S. 2000, MNRAS Robertson, B. et al. |
2006. ApJ Rubin. V. C. et al. | 2006, ApJ Rubin, V. C. et al. |
1979. ApJ | 1979, ApJ |
equation (19)) is solved numerically in order to obtain de/da. | equation \ref{dmless1}) ) is solved numerically in order to obtain $dv/dx$. |
The forth order. aclayslive Runge-Ixutta scheme was used to obtain solutions depicted on Figure l.- | The forth order, adaptive Runge-Kutta scheme was used to obtain solutions depicted on Figure 1. - |
Figure 4. | Figure 4. |
Acljusting rr,CIN rE we select (hose solutions which both satisfy. inner density condition. | Adjusting $x^{\rm CAK}_{c}$, $x^{\rm GEF}_{c}$ we select those solutions which both satisfy inner density condition. |
The following densities at (he inner boundaries were adopte: Pin10Zeemο [or ay=50. py,=10teem* for c,=100. pj,1016ecm* [or.r.= 500. pj,=10?!gem or c.=8000. | The following densities at the inner boundaries were adopted: $\rho_{in}=10^{-12}{\rm \,g\,cm^{-3}}$ for $x_c=50$ , $\rho_{in}=10^{-14}{\rm \,g\,cm^{-3}}$ for $x_c=100$, $\rho_{in}=10^{-16}{\rm \,g\,cm^{-3}}$ for $x_c=500$ , $\rho_{in}=10^{-21}{\rm \,g\,cm^{-3}}$ for $x_c=8000$. |
The comparative results oftje numerical integration of (19)) for s=1 (GEF solution) aud for s—0 (CAL wind theorv) are shown on Fig.l. | The comparative results of the numerical integration of \ref{dmless1}) ) for $s=1$ (GEF solution) and for $s=0$ (CAK wind theory) are shown on Fig.1. |
These solutions were obtained for the following set of parameters: The difference between GEF and CAIs wind is more pronounced when the considerable portion of the wind is accelerated at a distance less than 100r, from DII. | These solutions were obtained for the following set of parameters: The difference between GEF and CAK wind is more pronounced when the considerable portion of the wind is accelerated at a distance less than $100\,r_g$ from BH. |
Note that the terminal velocity changes form Neο=0.36 for v=50 do κους=0.19 for e.=500. | Note that the terminal velocity changes form $\Delta
v^{\infty}/v^{\infty}=0.36$ for $x_c=50$ to $\Delta
v^{\infty}/v^{\infty}=0.19$ for $x_c=500$. |
The obtained results show that the GEF flow can be sulliciently more fast than the flow which is described by CAI theory. | The obtained results show that the GEF flow can be sufficiently more fast than the flow which is described by CAK theory. |
It is illustrative to demonstrate that CAI solution max be obtained from (17)) by "switching off smoothlv the gravitational redshifting. | It is illustrative to demonstrate that CAK solution may be obtained from \ref{eqn1}) ) by "switching off" smoothly the gravitational redshifting. |
To obtain the continuous transition from the GEF solution to the CAI solution of equation (17)) the following procedure was adopted. | To obtain the continuous transition from the GEF solution to the CAK solution of equation \ref{eqn1}) ) the following procedure was adopted. |
We assumed that the radiation force im. (17)) is fy~ο.CM/r? The introduced parameter s continuously changes from 1 (GEF case) to O (CAN wind). | We assumed that the radiation force in \ref{eqn1}) ) is ${\displaystyle f_L\sim dv/dr+\frac{1}{c}\,s\,GM/r^2}$ The introduced parameter $s$ continuously changes from 1 (GEF case) to 0 (CAK wind). |
Numerically calculating solutions of (17)) for different values of s. applving (he inner density boundary conditions it is possible (ο demonstrate the continuous transition of these solutions rom the limiting cases of CAIs and GEF solutions. | Numerically calculating solutions of \ref{eqn1}) ) for different values of $s$, applying the inner density boundary conditions it is possible to demonstrate the continuous transition of these solutions from the limiting cases of CAK and GEF solutions. |
The resultsare shown on Figure 2. | The resultsare shown on Figure 2. |
The introduction of (he Paczvuski - Wiita ( PW ) (16)) potential. allows to simulate the effects of general relativity. | The introduction of the Paczynski - Wiita ( PW ) \ref{poten1}) ) potential, allows to simulate the effects of general relativity. |
Equations analogous to (19)). (25). (26)) are derived in Appendix. | Equations analogous to \ref{dmless1}) ), \ref{meq1}) ), \ref{meq2}) ) are derived in Appendix. |
The results of the numerical integration are shown on Figure4. | The results of the numerical integration are shown on Figure4. |
Introduction of the modified potential can give à gain in e* that varies from οον0.1 fora.=30 to Aesο~0.03 for 100. | Introduction of the modified potential can give a gain in $v^\infty$ that varies from $\Delta v^\infty/v^\infty\sim 0.1$ for$x_c=30$ to $\Delta v^\infty/v^\infty\sim 0.03$ for $x_c=100$ . |
Introducing the following nondimmentional | Introducing the following nondimmentional |
The linitations imposed bv the atmospheric sccing is a serious probeni for eround based observatious. | The limitations imposed by the atmospheric seeing is a serious problem for ground based observations. |
Speckle iuterferoimnetrv. which allows o1ο to circumvent blurring by the Earth's atimosphere. has beeu known for three decades. (Labeyiie 1970) aud is mainly applied to the research of close binary aud uultiple systems (see the laree series of papers by MeAlister aud collaborators). to the measurements of sellar diameters aud to the study of the strucure of circuustelar euvelopes at different wavelengths: it has been also uxxl to evaluate SIZCS and shapes of the iuiror objects of the solar svstoin. | Speckle interferometry, which allows one to circumvent blurring by the Earth's atmosphere, has been known for three decades (Labeyrie 1970) and is mainly applied to the research of close binary and multiple systems (see the large series of papers by McAlister and collaborators), to the measurements of stellar diameters and to the study of the strucure of circumstellar envelopes at different wavelengths; it has been also used to evaluate sizes and shapes of the minor objects of the solar system. |
Unfortunately. tus technique has not been widely applied so far since its major limitation lies in the relatively siuall cauce range alowed for the object magnitude. | Unfortunately, this technique has not been widely applied so far since its major limitation lies in the relatively small dynamic range allowed for the object magnitude. |
However. speckle interferonetry. under certain observiug conditious. can still be sce to retrieve the difference in magnitude between objects which are quite close in terms of relative brightuess, | However, speckle interferometry, under certain observing conditions, can still be used to retrieve the difference in magnitude between objects which are quite close in terms of relative brightness. |
Tn spectral aalysis. the flux from a composite object. when interpreted as due to a slrele source. wil most certainly cause confusion aud mw originate celalorate, but unrealistic. theories. | In spectral analysis, the flux from a composite object, when interpreted as due to a single source, will most certainly cause confusion and may originate elaborate, but unrealistic, theories. |
Such a confusing situalon 1s evident iu the class of the stars. Poplation I carly-A. recently extended up to earh-F type stars characterized by metal lines much weaker than ex)octed or their spectral type. | Such a confusing situation is evident in the class of the stars, Population I, early-A, recently extended up to early-F type stars characterized by metal lines much weaker than expected for their spectral type. |
The wide raice of the derive metal nuderabundances aud the variety «Xf explanations o the phenomenon are found in the large umber of receut yapers on the identification aud interpretation of these stars. | The wide range of the derived metal underabundances and the variety of explanations of the phenomenon are found in the large number of recent papers on the identification and interpretation of these stars. |
Farageianaao Bouitacio (1999) raised the qiestion hat undetected duplicitv is a pesible explauation of he peculiar Balmer profiles (shedloww cores aud broad wines) aud of the apparent ictal underabundauces of several candidates: in fact. in a composite spectrin. the veiling effect produces shallow lines which are characteristic of most stars (see Corbally 1987). | Faraggiana Bonifacio (1999) raised the question that undetected duplicity is a possible explanation of the peculiar Balmer profiles (shallow cores and broad wings) and of the apparent metal underabundances of several candidates; in fact, in a composite spectrum, the veiling effect produces shallow lines which are characteristic of most stars (see Corbally 1987). |
The speckle camera mounted on the Adaptive Optics module (AdOptaTNC) of the 3.511. Telescopio Nazionale Galileo (TNC) is expected to reach the diffraction. lint (QOIS at θά). aud is au ideal tool for separating narrow binary systems with magnitude differences between their components of less than 3 magnitudes. as is expected in the case of biuuitv of a cauclicdate. | The speckle camera mounted on the Adaptive Optics module (AdOptTNG) of the 3.5m Telescopio Nazionale Galileo (TNG) is expected to reach the diffraction limit $0\farcs{043}$ at 600nm) and is an ideal tool for separating narrow binary systems with magnitude differences between their components of less than 3 magnitudes, as is expected in the case of binarity of a candidate. |
The imager is an ICCD Proxitronic camera with a «quautuni efficiency optimized for the blue part of the visible spectrum (2:20% at 500uu). | The imager is an ICCD Proxitronic camera with a quantum efficiency optimized for the blue part of the visible spectrum $\approx20$ at 500nm). |
The central part of the TV sigwl is digitized iu a 128« pixel array (5 lits/px) at the staidiard frame rae of 25 Tz. while the single frame expostre ranges frou 2 to lms. | The central part of the TV signal is digitized in a $128\times128$ pixel array (8 bits/px) at the standard frame rate of 25 Hz, while the single frame exposure ranges from 2 to 40ms. |
Au optical relay provides a scale of zx ‘ps elvi ισα field oDview of 2:79... | An optical relay provides a scale of $\approx$ /px giving a field of view of $\approx$. |
No atiuosoherie dispersio1 correction is applied. | No atmospheric dispersion correction is applied. |
The speckle camera compues in realtime the power spectrin of cach frame and suns. directv the whole set of power spectra otained during the ru1 | The speckle camera computes in real–time the power spectrum of each frame and sums directly the whole set of power spectra obtained during the run. |
The daa are then offline correced for the iistruinental biases such as the backeround aud detector ithomogcucitics. | The data are then off–line corrected for the instrumental biases such as the background and detector inhomogeneities. |
The filter set includes some general purpose (Strónuugren bands) and some narrow bandpass ones (o8. IL, or TiO and ZrO absorption baud). | The filter set includes some general purpose (Strömmgren bands) and some narrow bandpass ones (e.g. $_{\alpha}$ or TiO and ZrO absorption bands). |
A detailed description of the real.time speckle facility can be found i Marchetti et al. ( | A detailed description of the real–time speckle facility can be found in Marchetti et al. ( |
1997) and. Mallucci (1998). while the realtine data acquisition is fully described in Baruffolo. Ragazzoni Farinato (1998). | 1997) and Mallucci (1998), while the real–time data acquisition is fully described in Baruffolo, Ragazzoni Farinato (1998). |
Acaibration run of the speckle camera of he TNG has heej uxed ο observe a suple of stars classified as from spectroscopic observations: this sample has been extracted from the list published by Farageianua Doniποιο (1999) and it is shown im Table Ll. | A calibration run of the speckle camera of the TNG has been used to observe a sample of stars classified as from spectroscopic observations; this sample has been extracted from the list published by Faraggiana Bonifacio (1999) and it is shown in Table \ref{tab:list}. |
We obtained speckle observations of these stars on the uights of December 20th and 21st. 1999 aud ou September 28th. 2000. | We obtained speckle observations of these stars on the nights of December 20th and 21st, 1999 and on September 28th, 2000. |
The nights were plagued by poor secine aud as | The nights were plagued by poor seeing and as |
absence of confirming lines if the line wereA3727.. oorLa. and the faint continuum ciscontinultv across the line. | absence of confirming lines if the line were, or, and the faint continuum discontinuity across the line. |
The redshift is based on a single emission line. which we interpret asΕναν. based. on the absence of confirming lines if the line were oorLa. and the faint continuum ciscontinultv across the line. | The redshift is based on a single emission line, which we interpret as, based on the absence of confirming lines if the line were, or, and the faint continuum discontinuity across the line. |
The redshift is based on a single emission line. which we interpret asΕναν. based. on the absence of confirming lines if the line wereA3727.. oorLa... and absence of continuum emission. | The redshift is based on a single emission line, which we interpret as, based on the absence of confirming lines if the line were, or, and absence of continuum emission. |
This is a tvpical example of a source in the "redshift desert. with dedetected at the very edge of the spectral coverage. | This is a typical example of a source in the `redshift desert', with detected at the very edge of the spectral coverage. |
The {line is ciffuse and extended. and the continuum emission is very strong. | The line is diffuse and extended, and the continuum emission is very strong. |
The redshift is confirmed by carbon lines. | The redshift is confirmed by carbon lines. |
Vhe continuum is well detected (Fig. 2)). | The continuum is well detected (Fig. \ref{continua}) ), |
but we see no emission or absorption lines. | but we see no emission or absorption lines. |
The rise in the continuum around. 77500 iis probably due to the bbreak at z~0.9. | The rise in the continuum around $\sim$ is probably due to the break at $z\sim 0.9$. |
The redshift is based on a single emission line. which we identify asA3727... based on the absence of confirming lines if the line wereLya.. oorlla.. and the presence of clear underlying continuum emission. | The redshift is based on a single emission line, which we identify as, based on the absence of confirming lines if the line were, or, and the presence of clear underlying continuum emission. |
The redshift is based on a single emission line. which we interpret asLya.. based. on the absence of confirming lines if the line wereA3727.. oorlla. and the continuum cdiscontinuity across the line. | The redshift is based on a single emission line, which we interpret as, based on the absence of confirming lines if the line were, or, and the continuum discontinuity across the line. |
Vhis source is at lower recshift than expected from the fyz relation (see also 85.2.3). | This source is at lower redshift than expected from the $K-z$ relation (see also 5.2.3). |
Both the redshift and identification of the radio source are secure. | Both the redshift and identification of the radio source are secure. |
Because no optical counterpart was detected down to f~25. we did not attempt to obtain a spectrum. | Because no optical counterpart was detected down to $I\sim25$, we did not attempt to obtain a spectrum. |
Because no optical counterpart was detected down to f~25. we did not attempt to obtain a spectrum. | Because no optical counterpart was detected down to $I\sim25$, we did not attempt to obtain a spectrum. |
In paper L. we have used rresolution radio images to identify the host galaxies of the USS sources in deep A band images (reaching ἐν=21 for the faintest sources). | In paper I, we have used resolution radio images to identify the host galaxies of the USS sources in deep $K-$ band images (reaching $K=21$ for the faintest sources). |
Previous USS searches have mostly used ~ rresolution radio maps2000).. ancl optical (2 or { band) or ἐν band imaging. | Previous USS searches have mostly used $\sim$ resolution radio maps, and optical $R-$ or $I-$ band) or $K-$ band imaging. |
Here we discuss the ellicicney of our identification procedure based on the data obtained to date. | Here we discuss the efficiency of our identification procedure based on the data obtained to date. |
]t is possible that our relatively low resolution racio maps may have Led to a higher fraction of mis-identifications. | It is possible that our relatively low resolution radio maps may have led to a higher fraction of mis-identifications. |
We can. however. use some prior information to determine if the spectroscopically observed object is the correct. host galaxy of the USS radio source. | We can, however, use some prior information to determine if the spectroscopically observed object is the correct host galaxy of the USS radio source. |
One important tool is the Llubble A diagram (see also 85.2.3). | One important tool is the Hubble $K-z$ diagram (see also 5.2.3). |
show that the hosts of radio galaxies are likely to be about 2 magnitudes brighter than normal star-forming ealaxies at the same redshift. | show that the hosts of radio galaxies are likely to be about 2 magnitudes brighter than normal star-forming galaxies at the same redshift. |
Coupled to the rarity of racio galaxies (c.g. 2001a)) compared with normal star-forming galaxies (ος. 2004)). this means that a mis-identification would most likely be made with a normal galaxy (as opposed to another radio galaxy host). several magnitudes fainter than expected for its redshift. | Coupled to the rarity of radio galaxies (e.g. ) compared with normal star-forming galaxies (e.g. ), this means that a mis-identification would most likely be made with a normal galaxy (as opposed to another radio galaxy host), several magnitudes fainter than expected for its redshift. |
Ln other words. the faintest near-LR (A= 19.5) galaxies in our | In other words, the faintest near-IR $K\geq19.5$ ) galaxies in our |
The recognition of the existence of stellar populations differius for age. clieinical conrpositiou. spatial distribution and kinematical properties has been the fundamental breakthrough iu the knowledge of galactic structure. and the basis for models of galaxy formation and evolution (sec. e.g.. the review by Alajewski 1993). | The recognition of the existence of stellar populations differing for age, chemical composition, spatial distribution and kinematical properties has been the fundamental breakthrough in the knowledge of galactic structure, and the basis for models of galaxy formation and evolution (see, e.g., the review by Majewski 1993). |
The large subsample of the Iipparcos catalogue for which radial velocity aud proper motions are available appears a promising tool to attempt a description of the local behaviour of stellar populations. | The large subsample of the Hipparcos catalogue for which radial velocity and proper motions are available appears a promising tool to attempt a description of the local behaviour of stellar populations. |
The erived database is lareclyOo incomplete aud heterogencous. and various steps will be necessary to ↴⋝↸∖⋜∏⋝↕↸∖↑∪↥⋅↸∖⋯⊳∐⋜↧↸⊳∪↕↸⊳↕∏↴ | The derived database is largely incomplete and heterogeneous, and various steps will be necessary to be able to reach a conclusion. |
∖↴↕∪↕∙∖∏↑∐≼↧⋯∖↸⊳⋜⋯↑↕∪∐∙↕↑↕↴∖↴ possible to form an idea of the variations in age and heavy element abundance with variations in kinematics. ic.. in the componcuts (VT. of star space velocity in the Galaxy. | With due caution, it is possible to form an idea of the variations in age and heavy element abundance with variations in kinematics, i.e., in the components $U,V,W$, of star space velocity in the Galaxy. |
The necessary information on metal coutet is obtained (for part of the selected objects) from existing catalogues. | The necessary information on metal content is obtained (for part of the selected objects) from existing catalogues. |
On the basis of these data aud of theoretical isoclrones we check that differences in ccorrespoud to the expected differences in|Fo/TI|:: this will allow to interprete the observed colour of the main sequence location in terms of metal content. | On the basis of these data and of theoretical isochrones we check that differences in correspond to the expected differences in: this will allow to interprete the observed colour of the main sequence location in terms of metal content. |
We crane also the behaviour of stellar orbit eccentricities as function of space velocity. which gives a picture of the local galactic structure consistent with the oue sugeested by star distribution as function of metal content. | We examine also the behaviour of stellar orbit eccentricities as function of space velocity, which gives a picture of the local galactic structure consistent with the one suggested by star distribution as function of metal content. |
The results we obtaim are valid for the solar uciehbourhood: in the limits in which this region is represcutative of the body of the galaxy. such results cau eive hints ou galactic structure on a larger scale. | The results we obtain are valid for the solar neighbourhood; in the limits in which this region is representative of the body of the galaxy, such results can give hints on galactic structure on a larger scale. |
We extracted from the Hipparcos Catalogue (ESA 1997) the single objects with an eror on the parallax oz/3 x 0.15 and ofBV) < GL. for which estimates of the radial velocity were found iu the literature (Turon et al. | We extracted from the Hipparcos Catalogue (ESA 1997) the single objects with an error on the parallax $\sigma_ \pi$ $\pi$ $\leq$ 0.15 and $\sigma(B~-~V)$ $\leq$ 0.1, for which estimates of the radial velocity were found in the literature (Turon et al. |
1992: Darbier-Drossat et al. | 1992; Barbier-Brossat et al. |
1001 Duflot et al. | 1994; Duflot et al. |
1995a.]: Fehreubach et al. | 1995a,b; Fehrenbach et al. |
1996. 1997). for a total of 9972 objects. | 1996, 1997), for a total of 9972 objects. |
When more than one value was found or au object. either the most recent or the one with the smallest error was chosen. | When more than one value was found for an object, either the most recent or the one with the smallest error was chosen. |
We accepted recognized periodic variables (total nunmiber 267). | We accepted recognized periodic variables (total number 267). |
We also considered single objects or Which o,/7 « 1 (total number about 15000. 810 oerodie variables) oulv for comparison purpose. | We also considered single objects for which $\sigma_\pi$ $\pi$ $<$ 1 (total number about 18000, 810 periodic variables) only for comparison purpose. |
knowu or suspected non-single stars have been excluded. on the sis of IHipparcos Catalogue iudicatious. | Known or suspected non-single stars have been excluded on the basis of Hipparcos Catalogue indications. |
The velocity sample obtained above is not complete aud suffers from many biases. which will be discussed in he following section. | The velocity sample obtained above is not complete and suffers from many biases, which will be discussed in the following section. |
Subsets and Splits
No saved queries yet
Save your SQL queries to embed, download, and access them later. Queries will appear here once saved.