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1. Polarization properties (transmitted radiation)
Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...
[ Сохраненная копия ]  Ссылки http://www.astro.spbu.ru/DOP/8-GLIB/ASTNOTES/node5.html -- 24.1 Кб -- 19.11.2010
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2. Determinations of Dust Scattering Properties
This is a tabulation of interstellar dust scattering properties dertermined from observations of various astrophysical objects (eg., ... Almost all studies in this field aim to determine the single scattering albedo (a) and scattering phase function asymmetry (g = <cos( )>) as different wavelengths. ... Plot Details . ... Plot details links to a page describing the studies included in the plot, the radiative transfer model used in each study, and an ascii listing of data plotted. ...
[ Сохраненная копия ]  Ссылки http://www.stsci.edu/~kgordon/Dust/Scat_Param/scat_data.html -- 6.5 Кб -- 28.11.2006
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3. The statistical properties of HSS BCGs
... The sky distribution of the BCGs from the HSS sample is shown in Fig. 6 together with BCGs from the SBS and Case surveys (Izotov et al. [ 1993b ]; Pustilnik et al. ... First, we compare the apparent magnitude distributions of the three samples. ... The similar behaviour of the faint end of the apparent magnitude distributions infers that the Northern BCG sample may have a similar completeness down to this limiting magnitude. ...
[ Сохраненная копия ]  Ссылки http://www.sao.ru/precise/Laboratory/Publications/1999/HSSI/TEXT/node20.html -- 7.3 Кб -- 24.11.1998
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4. Sample Properties
Next: Redshift Distribution Up: Sample Identification Previous: Previously Identified Sources . ... In Figure 3, we plot the redshift distribution of DXRBS FSRQs opposite that of the 1 Jy and S4 samples. In Figure 4, we plot the redshift distribution of DXRBS BL Lacs opposite the Slew and 1 Jy samples. ... The apparent deficit of objects at the very highest luminosities is a result of the smaller area of sky covered by DXRBS compared to, e.g., the Slew and 1 Jy samples. ...
[ Сохраненная копия ]  Ссылки http://www.eso.org/~ppadovan/survey/dxrbs_paper/node11.html -- 5.2 Кб -- 03.12.2003
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5. Vladimir Marsakov Abstracts
Authors: Yu.G. Shevelev , V.A. Marsakov , . ... We have constructed and investigated properties of metallicity function of disk stars with different ages, proceeding from the statistically restored real altitude distributions of stars at the solar galactocentric distance. It is shown that the metallicity distribution of stars in each age range is not of Gaussian form, but it may be considered as a superposition of two normal distributions centered at -0.2 and 0.0 dex. ...
[ Сохраненная копия ]  Ссылки http://ip.rsu.ru/~marsakov/abs/abst28.htm -- 4.1 Кб -- 02.02.2007
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6. Figures for Scattering Paper
Figure 1. ... Scattering geometry illustration. ... Maps of scattering angle in the cluster core for standard GCW grains and a Model A nebula (left) and UV-altered GCW grains in the same model (right). ... Degrees of consistency between the scattering angles of different models at different wavelengths. ... Schmidt scattering angles over a wider area. ... Schmidt line-of-sight separations over the same area, derived for two different simplified geometric models. ...
[ Сохраненная копия ]  Ссылки http://www.naic.edu/~gibson/papers/fig/pleiades/scat/ -- 6.8 Кб -- 16.05.2003
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7. STELLAR PROPERTIES
Next: EVOLUTION MODELS Up: EXTREME HELIUM STARS: PULSATION Previous: EXTREME HELIUM STARS . The characteristic surface properties, effective temperature , surface gravity and composition , of EHes have been summarized by Jeffery (1996). ... Helium: ( ) By definition, helium dominates the atmospheric abundances. ... This is supported by a correlation between N and Fe abundances in EHes. ... Next: EVOLUTION MODELS Up: EXTREME HELIUM STARS: PULSATION Previous: EXTREME HELIUM STARS Simon Jeffery . ...
[ Сохраненная копия ]  Ссылки http://star.arm.ac.uk/~csj/research/ehe_review/node2.html -- 8.5 Кб -- 25.01.2002
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8. http://xray.sai.msu.ru/~polar/html/publications/jenam98/abs
In this paper we review our results on the properties and evolution of isolated neutron stars. We calculate space distributions of these objects for different assumptions about the kick velocity and show, that the distribution has a torus-like structure. We calculate the evolution of isolated neutron stars with and without magnetic field decay and give characteristic parameters for these cases with applications to ROSAT X-ray sources. ...
[ Сохраненная копия ]  Ссылки http://xray.sai.msu.ru/~polar/html/publications/jenam98/abs -- 1.8 Кб -- 18.09.1998
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9. Spectral energy distribution
... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...
[ Сохраненная копия ]  Ссылки http://mavr.sao.ru/hq/ssl/IRAS04296/node8.html -- 17.5 Кб -- 02.10.2012
[ Сохраненная копия ]  Ссылки http://www.sao.ru/hq/ssl/IRAS04296/node8.html -- 17.5 Кб -- 01.10.2012
[ Сохраненная копия ]  Ссылки http://jet.sao.ru/hq/ssl/IRAS04296/node8.html -- 17.5 Кб -- 01.10.2012
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10. Clumpy dust disks
... Abstract: We present Monte Carlo radiative transfer simulations for spiral galaxies modelled as a stellar disk and a two-phase clumpy dust distribution. ... As a general result, clumpy models are less opaque than the corresponding homogeneous models. ... 0.00 0.15 0.50 0.1 0.5 1.0 2.0 5.0 10.0 0.25 X . ... We have also produced several homogeneous models, to compare to the clumpy models. ... Homogeneous and clumpy models with the same tauV have the same dust mass. ...
[ Сохраненная копия ]  Ссылки http://www.arcetri.astro.it/~sbianchi/clumping.html -- 14.5 Кб -- 29.03.2002
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11. http://www.gao.spb.ru/english/as/j2014/presentations/kudryashova.pdf
... St Petersburg 23, September 2014 1 Motivation · Origin of Martian moons? ... Considered error sources: ­ Phobos a priori ephemerides; ­ Phobos a priori GM value; ­ measurements noise; ­ different strategies; · Methods: ­ real data analysis; ­ simulations. ... St Petersburg 23, September 2014 8 Simulations: sensitivity of the measurements to the a priori GM value Simulations: zero noise+ IMCCE a priori ephemerides +GMPH = 7.16 * 105 m3/sec2. ... St Petersburg 23, September 2014 14 Thank you! ...
[ Текст ]  Ссылки http://www.gao.spb.ru/english/as/j2014/presentations/kudryashova.pdf -- 482.3 Кб -- 28.09.2014