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. ...

... 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 . ...

... Research . ... Laboratory . ... The software developed in the laboratory allows to carry out the whole cycle of the satellite information processing: the initial treatment of the data, coordinate relation, topside ionogram deduction, Ne(h) profiles calculation, global mapping the ionospheric parameters, ionospheric modeling and investigations of the mechanisms of the ionospheric parameters variations with local time, season, magnetic activity level, longitude, latitude, and altitude. ...

... 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. ...

... 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...

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. ...

... Example of an Association Table . ... CCD commands . ... ROMAFOT Command List . ... Commands of the context LONG . ... Command parameters (1) . ... Checklist of necessary table files . ... Observation Summary Table with file classifications appended in column :EXPTYPE and :OPATH as defined and applied in Table . ... Columns for star-catalog table files . ... Passband columns of the instrument table file . ... Detector columns of the instrument table file . ... Columns of the gain-table file . ...

FAMILIES AND SCATTERING . ... An important observation on the orbital distribution of irregular satellites is that satellite families at Saturn, Uranus and Neptune are not well defined. At Jupiter one finds 3-4 reasonably compact retrograde families, corresponding to each of the previously known retrograde irregulars and one prograde family. ... That is contrary to the current doctrine that very little has happened to these irregular satellite families following their collisional formation. ...

Magellanic Clouds in interaction evolutionary search for good models Adam Rzicka1, Jan Palous1, Christian Theis2 1Astronomical Institute, Prague; 2Institut fЭr Astronomie, Wien Idea investigate the LMC-SMC-Milky Way (MW) interaction by modeling the distribution of HI related to the Magellanic System (BrЭns et al. ... How much does the HI distribution tell about the LMC/SMC motion? ... It's all about proper motion... select a high-quality model (FF 0.5) and look around Tidal models don't work.. ...

. 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.