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. ...

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• Dependence on the Scenario Parameters and Initial Distributions
• Initial binary parameters
• Parameters of binary compact star evolution

... 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. ...

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• Recent Advances in Parameter Estimation in Astronomy with Poisson-Distributed
• Indexing and Searching Distributed Astronomical Data Archives

... 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...

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• Determination of atmospheric parameters and calculation of chemical composition

... 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 . ...

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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. ...

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• Model Fitting
• COS Instrument Handbook
• covar2ellipse.pro (JWST Pipeline routines in IDL)

... Main page . ... Main results . Data . ... webmaster@izmiran.ru . ... The main subject of the laboratory is investigation of the large-scale structure of the topside ionosphere. The researches are based on the vast bank of data of the Intercosmos-19, Cosmos-900, and Cosmos-1809 satellites. ... study of the large-scale inhomogeneous structure of the ionosphere, including the night-side and day-side main ionospheric trough, the day-side Muldrew trough, the ring ionospheric trough etc.; . ...

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• IZMIRAN - Laboratory for Physics and modeling of the ionosphere
• IZMIRAN - Laboratory for ionosphere discontinuity investigation: The

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.. ...

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• casacore: casa::Weibull Class Reference
• casacore: casa::Poisson Class Reference
• casacore: casa::Uniform Class Reference

. 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.

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• "STP Data" STP Data
• Index of /stp/data/Images_of_f-plots/TABL/Tables of different Parameters/M3000
• Index of /stp/data/Images_of_f-plots/TABL/Tables of different Parameters/fo E

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. ...

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• Preparation of parameter file
• Parameters
• FSRQs

To construct two-dimension distribution of minor planets user should specify elements/ parameters/ function that will be plotted as abscissas and ordinates. In three-dimension case one should add to them the element plotted on Z axis. ... Though you may choose elements plotted along different axes at will, often there is good reason to plot such elements as a, n, or n" along X axis (two-dimension distributions) and to plot them along Y axis in three-dimension case. ...

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• Keywords_262
• ENGAMPLE

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 ) ­ ...

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• http://www.gao.spb.ru/english/as/j2014/presentations/kudryashova.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/suvorkin.pdf
• http://www.gao.spb.ru/english/as/j2014/presentations/kurdubov.pdf

... A number of different statistical methods are used for estimating parameters from a data set. The most commonly used one is the least squares method which estimates a parameter by minimizing the function : . where y is the dependent and x the independent variables while f is a given function. ... The most important assumptions are that the errors in the dependent variable are normal distributed, the variance is homogeneous, and the independent variables have no errors and are uncorrelated. ...

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• Corrections to the probability distribution
• EXAMINE/ROMAFOT
• The main observational parameters

... Archives . ... Reduced and Processed Data . ... 2 distribution plays an incredibly important role in astronomical data analysis, but it is pretty much a black box to most astronomers. ... Comment ( RSS ) | ... I guess in the typical analysis we call chi2 a ?random variable? that follows the chi2 distribution: . ... where D(i) is the observed data, M(i) is the model predicted data and we ?silently? assume that D(i) is normally distributed and each i measurement is independent. ... Chandra Blog . ...

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• Comments on: chi-square distribution [Eqn] By: Alex By: vlk By: aneta By: aneta
• Comments on: [ArXiv] Identifiability and mixtures of distributions, Aug. 3,
• The AstroStat Slog Blog Archive [ArXiv] Identifiability and mixtures of

... 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. ...

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• ffit help file
• Irregular Satellite Research
• C. Refereed Journal Publications 2001

... 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. ...

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• Magnetic mapping
• Multipoint correlations of the solar wind parameters observed by several
• The plot of the magnetic conjugation's time distribution

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. ...

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• Optical static Fourier spectrometer
• Introduction to Plasma Physics
• ION AND ELECTRON ENERGY DETECTOR PAN-2

... S _t_c,f_c,(_t),c = . ... We refer to ( 10 ) as the ``Gaussian chirplet transform'' (GCT). One characteristic of the one-dimensional Gaussian window is that its TF energy distribution is a bi-variate Gaussian function. Therefore its TF energy countours are elliptical, so shearing the TF distribution along the time axis provides no new degrees of freedom that cannot be obtained by combinations of shearing along the frequency axis together with dilation. ...

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• Relationship Between Auto Chirplet FF Plane and Radon Transform
• Footnotes
• Tutorial on Fortran 90, Digital UNIX

... Space flight . ... Zero Gravity . ... Characteristics of a Complex Flight: . ... Characteristics of the Reduced Gravity (Lunar Gravitation): . ... Characteristics of the Reduced Gravity (Martian Gravitation): . ... Services / Zero Gravity: General description Technical description Flight parameters Photo gallery Price . ...

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... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

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• Polarization properties (transmitted radiation)
• Database of Optical Properties -- Level: subpage
• Database of Optical Properties -- Level: subsubpage

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. ...

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• Vladimir Marsakov Abstracts
• Population of Galactic globular clusters, tabl
• Scientific Directions Achievements