Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

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. ...

In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...

... 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...

ESTIMATIONS OF EFFECTIVE HEIGHT, SIZE AND BRIGHTNESS TEMPERATURE OF SOLAR CYCLOTRON SOURCES A.N. Korzhavin, T.I. Kaltman Special Astrophysical Observatory of RAS, Saint­Petersburg, Russia arles@mail.ru The modeling of microwave emission from a spot­associated cyclotron source was done to refine the method of estimations of e#ective brightness temperature, size and height above photosphere in the processing of RATAN­600 observations. ...

Next: Simulations Up: Maximum Likelihood Estimation of Previous: Introduction . The properties of an ensemble of faint galaxies can be defined by the distribution of the parameters of the models that best fit each individual object. ... The model also includes instrumental parameters, such as the sky background (estimated locally) and amplitude of the noise. ... The probability of the observed value is then computed for each pixel using the adopted error distribution. ...

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 . ...

... A list of spectrum files from a set of observations, referring to one RGS instrument and one spectral order. These spectra files must be produced using the attstyle=user and associated parameters from a call to rgsproc . ... A list of accompanying event list files, in the same order as the spectra files. ... If this parameter is set to yes, the spectra files of the input lists will be combined to produced a combined spectrum file each for both spectra and background spectra files. filermf . ...

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

... Future seminars . P a s t seminars . Seminar council . The emission time of Gamma-Ray Bursts" . A. Sanin (IKI) . ... The three new parameters of cosmic gamma-ray bursts are introduced: the emission time, the peak energy of the emission time spectrum and the cosmological invariant parameter. ... Using this distribution the "collective estimation" of the best fitting redshifts for the group of long bright gamma-ray bursts detected by BATSE experiment was found. ...

... 2014: . Suppression of cooling by strong magnetic fields in white dwarf stars . ... 69, 439, 2014. Evidence of supercritical accretion in SS433 . ... We discovered a flat portion (white noise) in the power spectrum of SS433 due to an abrupt increase of the disk thickness in the supercritical region. ... Both the hard X-ray radiation and the visual light are seen reflected from the walls of the funnel that forms in the wind of the supercritical disk of SS433. ... Archive . ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Quasi-stationary electron distributions for the different values of the particle escape time. ... The electron-cyclotron maser instability is widespread in the Universe, producing, e.g., radio emission of the magnetized planets and cool substellar objects. ... The model used takes into account the radiation escape from the source region and the particle flow through this region. ...

THE THERMAL RADIATION OF THE LUNAR SURFACE IN THE IR RANGE OF THE SPECTRUM (10-12 µm). ... 0.80 0.60 0.40 0.20 0.00 -0.20 -0.40 -0.60 -0.80 -0.80 -0.60 -0.40 -0.20 0.00 0.20 0.40 0.60 0.80 Fig.1 0.80 0.60 0.40 0.20 0.00 -0.20 -0.40 -0.60 -0.80 -0.80 -0.60 -0.40 -0.20 0.00 0.20 0.40 0.60 0.80 Fig.2 0.60 0.40 0.20 -0.00 -0.20 -0.40 -0.60 -0.60 -0.40 -0.20 -0.00 0.20 0.40 0.60 0.80 Fig.3 Indicatrix of the thermal radiation of the Moon (10.5-12.5 µ). ...

. This Directory contains Model of distribution of density, temperature and effective collision freguency of electrons. Yu.K.Chasovitin. 1998. This Directory contains The program RIM98 for calculating the parameters of the ionosphere to use the "Reference Ionospheric Model-98" (RIM-98).Yu.K.Chasovitin. 1998.

... Up: Data Analysis Tools, Techniques, and Software . Previous: Starfinder: a Code for Crowded Stellar Fields Analysis . Table of Contents - Subject Index - Author Index - PS reprint - . ... 216, Astronomical Data Analysis Software and Systems IX, eds. N. Manset, C. Veillet, D. Crabtree (San Francisco: ASP), 627 . ... Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732, Tucson, AZ 85726 . ...

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 ( ). ...

... We are using Canadian Galactic Plane Survey l 74.2њ, -3.6њ < b This poster gives preliminary results for a full-fledged analysis of the gas properties and distribution of HISA features in the CGPS. ... where T ON and T OFF are observed brightnesses on and off the HISA feature, T S is the spin or excitation temperature of the HISA gas, tau is its optical depth, T C is the continuum intensity, and p is the fraction of H I emission lying behind the HISA feature. ... GIF | ...

... It is found that the correlation coefficients between these two parameters calculated separately inside and outside the sunspot formation zone ±30 have cyclic variation and occur in anti-phase. This suggests different mechanisms of formation of the corona in the fields of small, medium, and large scales. ... The relationship between the coronal green line brightness (CGLB) and the magnetic field strength (MFS) has been investigated by constructing the corresponding synoptic maps for the 1977-2001. ...

... Guider functions . ... Guide Sensor Performance . ... Guide Sensor Sky Coverage/ Star Availability . Guide Star Selection Criteria . ... Guide fiber organization and reach at plug plate . ... Plug plate holes for guide stars are identical to those for science FO . ... FOV for each of 9 guide stars is 7.4 arcsec dia. (0.45 mm FO, Sumitomo IGN-05/10) . ... Selected guide stars must have no neighbor stars within TBD (5 arcsec) radius that have a brightness within TBD (5 mag.) of guide stars . ...

... 3D structure rings , spots filaments · Application to Cygnus A and 3C 317 Radio cocoon and shaped Xray gas (contours) in Cygnus A Cygnus A (Chandra archive, courtesy P. Strub) large cocoon width elliptically shaped cluster gas marks bow shock axis ratio: 1.2 Outline · · · ­ Pretty data: Cygnus A Parameters of jet simulations in the history Extension to very low ... L g[ = -2 ] Parameter Study: Axis Ratio Small jets have spherical bow shocks! critical radius depends on . ...