... Method A simple radiative transfer model representing a HISA cloud with fore­ ground and background H i emission and background continuum emission is described by the expression T ON - T OFF =  T S - T C - p T OFF   1 - e -#  , (1) where T ON and T OFF are observed brightnesses on and o# the HISA feature, T S is the spin or excitation temperature of the HISA gas, # is its optical depth, T C is the continuum intensity, and p is the fraction of H i emission lying behind the HISA feature. ...

... Observations of the Moon eclipse on 17.09.97 have shown the Moon details contrasts had decreased and the total radio brightness had fallen at all observed frequency range (from 10% at 1.38 sm down to 2.5% at 13 sm). The fall of the Moon radio brightness has been detected during the eclipse at decemeter waves for the first time. ... Radio emission of the Copernicus crater at 1.38 and 2.7 sm has been detected for the first time. ...

... 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. ...

SAI 175 anniversary . ... Moscow University . Search for in SAI Moscow University Search for in Russian astronomical resources . ... SAI Astronomical Databases . ... Browse SAI Software archive(ftp.sai.msu.su) . ASTRONET.RU - Russian Astronomical Network (available in translit also) . ... SAI Supernovae Research Group . ... Department of the Galaxy and Variable Stars (in Russian) . Sternberg Astronomical Institute Seminars . ... All-Russian Astronomical Olympiad (in Russian) . ...

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. ...

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 ( ). ...

Old subtables of the extended ``HIPASS Bright Galaxy Catalog'' . ... Koribalski, Staveley-Smith, Kilborn, + HIPASS/ZOA teams 2004, AJ 128, 16 . The 1000 Brightest HIPASS Galaxies: HI Properties . ... The 1000 Brightest HIPASS Galaxies: The HI Mass Function . ... The 1000 Brightest HIPASS Galaxies: Newly Cataloged Galaxies . ... To download the gzipped ps-file click here . ... The Brightest Galaxies from HIPASS . Presented is the distribution of the 700 brightest HIPASS galaxies. ...

Next: Pulsations Up: PHYSICAL CHARACTERISTICS Previous: PHYSICAL CHARACTERISTICS . The fundamental properties of RCBs may be deduced from their spectra at maximum light. ... The properties of a stellar atmosphere may be measured from both the large-scale features - the broad-band flux distribution - and the detailed spectrum of absorption lines. ... They show that, in general, hydrogen makes up less than one part per thousand down to less than one part per million of the stellar atmosphere. ...

FEATURES OF THE HYDROGEN DISTRIBUTION AROUND LUNAR CRATERS PROCLUS AND KEPLER. ... In result of analysis of the data Lawrence and Feldman constructed the hydrogen distribution on the lunar surface [1]. ... However, the authors shown, that EN flux data features may be explained by other element abundance in the lunar soils, namely: Si, Ca, Gadolinium (Gd), Samarium (Sm) and Fe. ... Using of the Feldman's interpretation of the Lunar Prospector data [8], we constructed hydrogen distribution map (Fig.1). ...

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. ...

... 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. ...