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. ...

Еще в разделе: (Показать все результаты (>768) - xray.sai.msu.ru/ )

• Initial binary parameters
• Dependence on the Scenario Parameters and Initial Distributions
• Effect of sources evolution on

Stellar Clusters are very useful laboratories for empirically studying stellar evolution. ... All cluster stars are at the same distance . All cluster stars have the same physical age . ... CM diagram Young Cluster In this case we see the Main Sequence fully represented. The blue dots represent massive stars with short main sequence lifetimes. ... Thus, identifying the most massive star which is still on the main sequence is an effective means of determining the age of a stellar cluster. ...

Еще в разделе: (Показать все результаты (>430) - zebu.uoregon.edu/ )

• Radiation Dominance in the Early Universe

The radial distribution of metallicity of star-forming galaxies in a galaxy cluster can inform us about the mass assembly and enrichment history of the galaxy cluster. ... Both galaxy clusters are cool-core clusters at redshift z т?? ... The gas-phase metallicity of star- forming galaxies in MACS1115+01 exhibit anti-correlation with projected distance т??0.15 ТБ 0.08 dex/Mpc, whereas the radial metallicity distribution of RXJ1532+30 is statistically flat (т??0.09 ТБ 0.12 dex/Mpc). ...

Еще в разделе: (Показать все результаты (>731) - www.mso.anu.edu.au/ )

• http://www.mso.anu.edu.au/seminars/abstracts/20151106-1420.html

... 145Slee,Roy Savage We present detailed radio and optical parameters for the stronger radio sources in 58 Abell cluster fields observed with the Very Large Array (VLA) using scaled arrays at 1.5 and 4.9 GHz. ... The cluster fields were distributed over 24 h of RA and between declinations +35 deg and -30 deg. ... Optical identifications Cluster Source Radio Centroid Optical Position EF Ang. ...

Еще в разделе: (Показать все результаты (>2445) - www.sao.ru/ )

• HyperLEDA documentation: parameter: vdis
• A VLA Survey of Rich Clusters of Galaxies III
• A 20 cm VLA survey of Abell clusters of galaxies

. N OTE: . Only clusters with R<60 kpc were used to compute the spatial parameters and metallicity gradients for all subsystems except the corona. The numbers in parantheses give the number of clusters for which the corresponding parameter is known. The X O scale length of the old halo is strongly distorted by the observed asymmetry of the distribution of the corresponding clusters projected onto the XY plane ( Fig. 4А ) . discussion in the text | previous table .

Еще в разделе: (Показать все результаты (>139) - ip.rsu.ru/ )

• Vladimir Marsakov Abstracts
• Vladimir Marsakov Publication List
• Population of Galactic globular clusters, figures

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. ...

Еще в разделе: (Показать все результаты (>18230) - www.stsci.edu/ )

• HST this week: 215
• Hubble Space Telescope Observations of Globular Clusters in M87 and an Estimate
• HST this week

J/AstL/vol/page SAI Open Clusters Catalog (Glushkova+, 2009) ================================================================================ Automated search for star clusters in large multiband surveys. ... Color excesses E(B-V), distance moduli and ages were determined for 141 new and 27 known, but poorly studied clusters. We present the Sternberg Astronomical Institute Open Clusters Catalog (SAI OCL Catalog) of coordinates, diameters and main physical parameters of these clusters. ...

Еще в разделе: (Показать все результаты (>222) - ocl.sai.msu.ru/ )

• SAI Open Star Clusters (SAI OCL) Catalog
• SAI OCL Catalog Description
• SAI OCL Catalog Structure

... 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...

Еще в разделе: (Показать все результаты (>1106) - jet.sao.ru/ )

• harak_e
• Determination of atmospheric parameters and calculation of chemical composition

... Subject and Problems of Stellar Astronomy. ... Plane of Galaxy, Methods of Its Location Determination. ... Stars Distances. ... Other Methods of Stars Distances Determination. ... Tangential Velocities, Their Determination by Self-Motions. ... Determination of Solar Apex and Spatial Velocity by Radial and Spatial Velocities of Stars. ... Features of Orientation and Parameters of Peculiar Stellar Velocities Ellipsoid. ... General and Selective Light Absorption in Galaxy. ... Darc Clouds in Galaxy. ...

Еще в разделе: (Показать все результаты (>131) - space.univ.kiev.ua/ )

• Extragalactic Astronomy

The new view on the population of Galactic open clusters A.E.Piskunov1, N.V.Kharchenko2, S.RЖser3, E.Schilbach3, R.-D.Scholz4 1 2 3 4 Institute of Astronomy, Moscow, Russia Main Astronomical ... Observatory, Kiev, Ukraine Astronomisches Rechen-Institut, Heidelberg, Germany Astrophysikalisches Institut Potsdam, Germany What are open clusters and what do they teach us Groups of Population I ... Cluster complexes: OCC-1 = Gould's Belt cluster complex? ...

Еще в разделе: (Показать все результаты (>5) - www.gpad.ac.ru/ )

... Colours of stars and galaxies hold information on intrinsic and extrinsic parameters, such as stellar temperatures and galaxy populations, selective absorption and colour changes due different dust contents and inclination angles of galaxies, as well as galaxy redshifts and evolution. ... The colour magnitude diagram of 65000 galaxies to which all above-mentioned quantities and others contribute can only be explained by comparison with simulations. ... Colours are also of technical help. ...

Еще в разделе: (Показать все результаты (>66429) - www.eso.org/ )

• IAU Symp317 Scientific Program
• Marina Rejkuba's Web Site
• ESO - star07

... Archives . ... my first AAS. ... I was questioned by two attendees, acquainted before the AAS, if I can suggest them clustering methods relevant to their projects. ... classification vs. clustering or supervised learning vs. unsupervised learning : the former terms from the pairs indicate the fact that the scientist already knows types of objects in his hands. ... Tags: Classification , clustering , cosmology , spatial statistics , supervised learning , test , unsupervised learning . ...

Еще в разделе: (Показать все результаты (>3903) - hea-www.harvard.edu/ )

• Rotation Periods of ZAMS Stars
• The AstroStat Slog Blog Archive The LRT is worthless for ?
• Rotation Periods of PMS Stars

... 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. ...

Еще в разделе: (Показать все результаты (>2870) - star.arm.ac.uk/ )

• Galactic distribution and absolute magnitudes
• White Dwarf Merger Movie
• Irregular Satellite Research

... 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. ...

Еще в разделе: (Показать все результаты (>1875) - www.adass.org/ )

• Mapping the Jagiellonian Field of Galaxies
• Clustering Analysis Algorithms and Their Applications to Digital POSS-II
• Using Massively Parallel Processing of a NLTE Spectrum Synthetic Code and an

... 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. ...

Еще в разделе: (Показать все результаты (>338) - www.astro.spbu.ru/ )

• Introduction
• Model realization and some results
• Model of clusters

... For an input list of EBOXDETECT source locations, simultaneous maximum likelihood PSF fits to the source count distribution are performed in all energy bands of each EPIC telescope. A description of the main properties of the detection algorithm may be found in Cruddace, Hasinger, Schmitt (1988). ... Note, that =1 in the case of the individual energy band detection likelihoods listed in source table rows with ID_BAND 0 and is equal to the total number of energy bands in the ID_BAND=0 summary rows. ...

Еще в разделе: (Показать все результаты (>15095) - xmm.vilspa.esa.es/ )

• Parameters

... Programme . ... Abstract: Globular clusters can probe the formation history of galaxies by providing evidence for the chemical evolution and major episodes of star formation in their host galaxies, by examining their kinematic signatures, as well as their structural parameters. ... The giant elliptical NGC 5128 (Centaurus A), at a mere 4 Mpc away, gives us the only opportunity to study in extensive detail the globular cluster system of a recent merger galaxy. ...

Еще в разделе: (Показать все результаты (>13566) - www.atnf.csiro.au/ )

• Polarization/Stokes Handling (stokes and select)
• User Parameters - Pipeline & job control CentralProcessor 0.11 documentation
• imgen

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. ...

Еще в разделе: (Показать все результаты (>729) - www.ipa.nw.ru/ )

• ENGAMPLE
• Keywords_75

... Observatory . ... The Laboratory of Astrometry . Dept. for Physics of Stars&Galaxies . ... Astronomical Calendar . ... UkrVO . ... The purpose of research: Creating a stellar catalog to study the structure and kinematics of star systems, including open star clusters and stars with large proper motions; the enhancement ICRF / Hipparcos system to stars dawn to 17 m (V); Search of binary systems of brown dwarfs and determination of their parameters; astrometry of minor bodies of the Solar System. ...

Еще в разделе: (Показать все результаты (>578) - www.mao.kiev.ua/ )

• Achievements - Page 4
• Dept. for Physics of Stars&Galaxies

... We address a question if globular clusters (GC) in a protogalaxy could for some time evolve chemically as isolated systems, enriching themselves with heavy elements produced in first supernova events that follow initial star formation. We determine both the critical mass of a protoglobular cluster that is needed to retain the ejecta of the very first supernova, and the critical energy (i.e., number of supernovae) that is needed to expel the residual gas from a cluster of a given mass. ...

Еще в разделе: (Показать все результаты (>44) - www.inasan.rssi.ru/ )

• On current distance scales for open clusters
• Star Formation History