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1. Parameters of binary compact star evolution
... Figure: Massive binary evolutionary track. ... A short glance to this track is sufficient to understand that there are a lot of evolutionary scenario parameters, which affect different stages of the binary evolution. Fortunately, a very limited number of parameters has effect on the compact binary merging rate. ... The most important (and practically unique) parameter changing the galactic binary NS merging rate is the distribution of an additional (kick) velocity imparted to NS at birth. ...
[ Сохраненная копия ]  Ссылки http://xray.sai.msu.ru/~lipunov/kionewht/node9.html -- 7.2 Кб -- 16.06.2000
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2. Vladimir Marsakov Publication List
Scale-heights of the Galactic disk subsytems with different ages and metallicities . V.Marsakov & Yu. ... It is based on the fact, that all stars cross the disk plane several times during their Galactic orbital period. ... We have used our representative sample of nearby disk F2-G2 stars Marsakov & Shevelev (1995) in which fundamental stellar parameters was determined on the basis of published date on uvby-photometry, proper motion and radial velocities. ... Marsakov V.A., Shevelev Yu.G. Bull. ...
[ Сохраненная копия ]  Ссылки http://ip.rsu.ru/~marsakov/conf/paper1/conf1_1.htm -- 9.3 Кб -- 02.02.2007
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3. IAU Symp317 Scientific Program
Topics covered by the IAU Symp. ... Do all galaxies have stellar halos? ... Stellar tracers of the MW halo and nearby galaxies; the stellar population of star clusters and their contribution to the galaxy halos . ... NEW: Scientific program of the IAU Symposium 317 can be downloaded here . ... GLOBAL PROPERTIES OF STELLAR HALOS FROM THE MILKY WAY TO EXTERNAL GALAXIES . ... DISCRETE CONSTITUENTS OF STELLAR HALOS IN THE MILKY WAY AND IN EXTERNAL GALAXIES : PLANETARY NEBULAE and GLOBULAR CLUSTERS . ...
[ Сохраненная копия ]  Ссылки http://www.eso.org/~marnabol/IAU317_Scienpro_04012015.html -- 11.6 Кб -- 06.05.2015
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4. Astronomy HyperText Book: Stellar Evolution
... Stellar Evolution is driven entirely by the never ending battle between Pressure and Gravity . As imbalances are reached, the star is driven to find a new Energy source. ... Pressure and gravitational forces are equal, the star is stable and its core is sufficiently hot to fuse Hydrogen into Helium More about main sequence stars . ... The luminosity generated by the core fusion of Helium into Carbon is far greater than the shell luminosity associated with the fusion of Hydrogen into Helium. ...
[ Сохраненная копия ]  Ссылки http://zebu.uoregon.edu/textbook/se.html -- 4.8 Кб -- 16.12.1997
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5. Fundamental Parameters, Integrated Red Giant Branch Mass Loss, and Dust
Fundamental parameters and time evolution of mass loss are investigated for post-main-sequence stars in the Galactic globular cluster 47 Tucanae (NGC 104). ... We confirm the cluster's distance as d = 4611+213 -200 pc and age as 12 ТБ 1 Gyr. Horizontal branch models appear to confirm that no more red giant branch mass loss occurs in 47 Tuc than in the more metal-poor Я? Centauri, though difficulties arise due to inconsistencies between the models. ...
[ Сохраненная копия ]  Ссылки http://www.stsci.edu/~kgordon/papers/2011ApJS..193...23M.html -- 4.3 Кб -- 21.01.2016
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6. http://www.mrao.cam.ac.uk/galevol/jsabater-Cambridge.pdf
... 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Nuclear activity and environment Effect of environment on AGN is not completely clear yet. ... 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Effect of the mass Mass slices ­ optical and radio AGN overall interaction one-on-one interaction relative location 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Stratified study Stratifed study that considers several strata of mass. ...
[ Текст ]  Ссылки http://www.mrao.cam.ac.uk/galevol/jsabater-Cambridge.pdf -- 1542.2 Кб -- 06.10.2013
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7. Bias-Free Parameter Estimation with Few Counts, by Iterative Chi-Squared
... We demonstrate through numerical simulations that model parameters estimated with our technique are essentially bias-free, even when the average number of counts per bin is 1. ... The IW technique avoids such biases by estimating through successive iterations, where for each iteration, j, , and the best-fit parameters are determined by minimization of . ... In our sample, we find that the minimum values and best-fit parameters converge after about 6 iterations. ...
[ Сохраненная копия ]  Ссылки http://www.adass.org/adass/proceedings/adass94/kearnsk.html -- 12.3 Кб -- 03.11.2000
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8. "Structure" publications in 1996 year
Our publications in 1996 year . Lindner, U.; Einasto, M.; Einasto, J.; Freudling, W.; Fricke, K.; Lipovetsky, V.; Pustilnik, S.; Izotov, Y.; Richter, G. Astronomy and Astrophysics, v.314, p.1-12 (10/1996) . Thuan, Trinh X.; Izotov, Yuri I.; Lipovetsky, Valentin A . ... Edited by Daniel Kunth, B. Guiderdoni, M. Heydari-Malayeri, and Trinh Xu Thuan, 1996., p.607 . ... Edited by Daniel Kunth, B. Guiderdoni, M. Heydari-Malayeri, and Trinh Xu Thuan, 1996., p.587 . ... Thuan, Trinh Xuan; Izotov, Yu. ...
[ Сохраненная копия ]  Ссылки http://www.sao.ru/precise/Laboratory/Publications/1996_pub.html -- 5.7 Кб -- 28.06.2004
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9. Search for distant radio galaxies in SAO
... The search for distant objects which can be both galaxies and quasars is one of the most important problems of observational astrphysics, because it allows one to determine cosmological parameters connected with the time of appearence and evolution of stellar systems, large scale structure of the Universe. ... Radio galaxies are important objects to be studied because they are sources of infrared-optical-ultraviolet continuum, emission lines and continual radio emission. ...
[ Сохраненная копия ]  Ссылки http://mavr.sao.ru/hq/lran/vo/hzrgE.html -- 9.3 Кб -- 02.10.2012
[ Сохраненная копия ]  Ссылки http://www.sao.ru/hq/lran/vo/hzrgE.html -- 9.3 Кб -- 01.10.2012
[ Сохраненная копия ]  Ссылки http://jet.sao.ru/hq/lran/vo/hzrgE.html -- 9.3 Кб -- 01.10.2012
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10. Informational system "Evolution of RG"
The project of the informational system creation on the problem of evolution of radio galaxies, as a part of the "Big Trio" project aimed on studing of distant radio galaxies, is designed. This system allows a user to operate with simulated curves of spectral energy distributions (SED) to estimate ages and redshifts by photometry data. Authors use SEDs of several models for different types of galaxies. ... The HTTP and e-mail access is organized to this system. ...
[ Сохраненная копия ]  Ссылки http://www.sao.ru/sed/ -- 4.7 Кб -- 15.07.2001
[ Сохраненная копия ]  Ссылки http://sed.sao.ru/ -- 4.7 Кб -- 15.07.2001
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11. Structure of the Spectral Package
... Several of the tasks in the spectral package share a common set of parameters. ... Each task in the spectral package has a hidden parameter which points to the pkgpars parameter file. The parameters stored here include the observed data sets and the model descriptor, and instrument-specific parameters. ... The observed counts and error data set contained in the table file ( *_obs.tab ) produced by qpspec will be the input data for subsequent spectral tasks. ...
[ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/PROS/PUG/node140.html -- 9.0 Кб -- 01.10.2012
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12. The HIPASS Bright Galaxy Catalog
Old subtables of the extended ``HIPASS Bright Galaxy Catalog'' . ... Koribalski, B.S. 2002, in ``Seeing Through the Dust'', ASP Conf. ... The Brightest Galaxies from HIPASS . Presented is the distribution of the 700 brightest HIPASS galaxies. ... Koribalski, Staveley-Smith, Kilborn, Ryder and the HIPASS/ZOA teams, ATNF Annual Report 2000 . ... The 1000 Brightest HIPASS Galaxies: New Galaxies . ... The 1000 Brightest HIPASS Galaxies: Extended Galaxies and Groups . ...
[ Сохраненная копия ]  Ссылки http://www.atnf.csiro.au/research/multibeam/HIPASS-BGC/tables/BGC.html -- 7.5 Кб -- 25.12.2007
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13. http://www.gao.spb.ru/english/as/j2014/presentations/guseva.pdf
Some peculiarities of orbits of observed comets. ... Icarus, 2005 Simulation and reality Distribution of anti-perihelia of short-period comets with e 0.9 ( ecliptic coordinates ) Distribution of anti-perihelia of short-period comets with e 0.9 ( ecliptic coordinates ) Distribution of anti-perihelia of long-period comets with 0.9 e 1 ( ecliptic coordinates ) ­ ...
[ Текст ]  Ссылки http://www.gao.spb.ru/english/as/j2014/presentations/guseva.pdf -- 1689.7 Кб -- 28.09.2014
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14. Abstract
Meteor outburst profiles and cometary ejection models . ... The spatial structure of meteor streams, and the activity profiles of their corresponding meteor showers, depend firstly on the distribution of meteoroid orbits soon after ejection from the parent comet nucleus, and secondly on the subsequent dynamical evolution. ... This paper describes how a trail cross section can be calculated once an ejection model has been assumed. ...
[ Сохраненная копия ]  Ссылки http://star.arm.ac.uk/~dja/papers/abs08EMP.html -- 2.5 Кб -- 18.04.2008
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15. research field
... Together, this small group works mostly in the field of Active Galactic Nuclei, exploring their distribution in parameter space (black hole mass, black hole spin, accretion rate) and their evolution in cosmic time. Since the growth and activity of the central black hole, on the one side, and the assembly of the host galaxy, on the other, go very tightly in parallel, the AGN evolution is a convenient window on the more general problem of the formation of cosmic structures. ...
[ Сохраненная копия ]  Ссылки http://www.arcetri.astro.it/science/gal-agn/res_salvati.html -- 2.2 Кб -- 14.08.2009
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16. Future of the Galaxy
... We consider the astrophysical evolution of the Galaxy over large time scales, from early stages (an age of ~10 8 yrs) to the end of traditional stellar evolution (~10 11 yrs). ... In the model considered, the basic stages of Galactic evolution are as follows. ... Essentially all other basic parameters of the Galaxy vary little. ... The final "stellar epoch" in the life of the Galaxy is completed ~10 13 yrs after its formation, when the evolution of the least massive stars comes to an end. ...
[ Сохраненная копия ]  Ссылки http://www.inasan.rssi.ru/~dwiebe/abstracts/future.html -- 3.7 Кб -- 27.09.2012
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17. Parameters
... Default . ... The descriptions below focus on the meaning of each filename parameter, leaving the exact details of the inferred default value to be explained in the algorithm section. evlist . ... file . The response matrix file (OGIP-compliant format). ... If a spectrum file is not provided ( withspectrum =no) this parameter specifies the INDEX number of a source in the source description list (parameter srclist ), and thereby the incidence angle and selection regions for the response matrix. ...
[ Сохраненная копия ]  Ссылки http://xmm.vilspa.esa.es/sas/6.1.0/doc/rgsrmfgen/node4.html -- 14.7 Кб -- 22.11.2004
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18. Theoretical Astrophysics
Subject, Problems and Objects of Theoretical Astrophysics. ... Stellar Photospheres, Their Features. ... Physics of Continuous Radiation Absorption in Stellar Photospheres. ... Continuous Radiation Absorption in Stellar Photospheres of Various Spectral Classes. Solar Type Photospheres. ... Characterisics of Absorption Lines. ... Interstellar Absorption Lines, Their Features. ... Physical and Dynamic Features of Interstellar Medium, Which Follows from Observations of Interstellar Absorption Lines. ...
[ Сохраненная копия ]  Ссылки http://space.univ.kiev.ua/courses/teor_astroph_e.html -- 8.7 Кб -- 23.02.2005
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19. PhSRM
MARS-96 . ROBOTIC SPACECRAFT MISSION TO MARS. ... The main scientific objectives of this mission are to investigate the evolution of Mars, that is, of its atmosphere, its surface, and its interior. ... abundance of minor components in the atmosphere (H2O, CO, O3 , etc), their variation and vertical distribution, and searches for regions with higher humidity; . ... Plasma: . ... the 3D distribution function; the ion and energy composition of plasma (near Mars and during interplanetary cruise); . ...
[ Сохраненная копия ]  Ссылки http://www.iki.rssi.ru/mars96/02_mars_e.htm -- 6.1 Кб -- 22.03.2002
[ Сохраненная копия ]  Ссылки http://www.cosmos.ru/mars96/02_mars_e.htm -- 6.1 Кб -- 22.03.2002
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20. http://selena.sai.msu.ru/San/Publications/ms38/ms059.pdf
... The analysis shows, that asteroid ­ rubble pile loses its fast fragments in no time but the retaining fragments forms a compact structure immersed in dust ­ gas atmosphere, created by interaction of interplanetary medium with dispersed product of collisional evolution of asteroid. By interaction of an asteroid ­ rubble pile with interplanetary medium structures asteroid can increase its brightness on account of blowed up dust simulating phenomenon of distant comet's brightening. ...
[ Текст ]  Ссылки http://selena.sai.msu.ru/San/Publications/ms38/ms059.pdf -- 155.0 Кб -- 06.10.2008
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