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. ...

... 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Nuclear activity and environment Effect of environment on AGN is not completely clear yet. ... 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Effect of the mass Mass slices ­ optical and radio AGN overall interaction one-on-one interaction relative location 05/09/2013 Galaxy Evolution over Five Decades - Cambridge 2013 Stratified study Stratifed study that considers several strata of mass. ...

... CentralProcessor 0.11 documentation . Calibration and Imaging Documentation . The cmodel pipeline task is responsible for extracting a local sky model (LSM) from the global sky model (GSM) and building an image from the components and/or images resulting from the request. ... MPI wrapper> cmodel -c config.in . ... None . ... If Cmodel.gsm.database is set to asciitable then a row/column (space separated) file is used as the global sky model source. ... cmodel (Model Image Generator) . ...

Next: CAL_getBoresightMatrix Up: Routines of the Calibration Previous: List of CCF Components Contents . ... The CAL functions CAL_getBadPixelList & CAL_getBadPixelMap use the CAL state variable temperature only to check that the current operating temperature is consistent with the CCF constituent BadPix . ... Used CAL State Variables . List of CCF Components used . ... Next: CAL_getBoresightMatrix Up: Routines of the Calibration Previous: List of CCF Components Contents Michael Smith 2011-09-20 ...

Topics covered by the IAU Symp. ... Do all galaxies have stellar halos? ... Stellar tracers of the MW halo and nearby galaxies; the stellar population of star clusters and their contribution to the galaxy halos . ... NEW: Scientific program of the IAU Symposium 317 can be downloaded here . ... GLOBAL PROPERTIES OF STELLAR HALOS FROM THE MILKY WAY TO EXTERNAL GALAXIES . ... DISCRETE CONSTITUENTS OF STELLAR HALOS IN THE MILKY WAY AND IN EXTERNAL GALAXIES : PLANETARY NEBULAE and GLOBULAR CLUSTERS . ...

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. ...

Find Similar Abstracts (with default settings below ) . ... Also-Read Articles . ... Parameters of the 41 Dra system components . ... 00/2001 . ... Stars: Binaries, Binaries: Fundamental Parameters, Binaries: Individual . ... 61B Based on spectral and speckle-interferometric observations of the system 41 Dra, model atmosphere parameters of the system components have been derived: component Aa - T eff = 6500K, lg g = 3.99, R = 1.87 R solar , component Ab - T eff = 6500K, lg g = 4.11, R = 1.61 R solar . ...

... 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 . ...

... 8, ``Celestial Mechanics'', 2002 On figure of a sublimating cometary nucleus Yu. D. Medvedev Institute of Applied Astronomy, St. Petersburg, Russia The problem of the change of the figure of a cometary nucleus when its matter is sublimating from the nucleus surface is considered. ... The evolution of the nucleus figure and rotational parameters is considered taking into account the dust component in the cometary matter. ... D. Evolution of form sublimating cometary nucleus. ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . Despite our knowledge of stellar evolution, star birth remains a mystery. ... The latter two may indicate the envelope mass, M(env) and jet power L(jet), respectively. ... Here is a supplementary diagram showing the evolution of a low mass star with a 3000 year, 90 per cent oscillation in accreting mass superimposed. ... Also available is the evolution of a 0.5 solar mass star (on request). ...

... We consider the astrophysical evolution of the Galaxy over large time scales, from early stages (an age of ~10 8 yrs) to the end of traditional stellar evolution (~10 11 yrs). ... In the model considered, the basic stages of Galactic evolution are as follows. ... Essentially all other basic parameters of the Galaxy vary little. ... The final "stellar epoch" in the life of the Galaxy is completed ~10 13 yrs after its formation, when the evolution of the least massive stars comes to an end. ...

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. ...

... Minute Values of Geomagnetic Field Components . ... AA 1868 - Present (3 hourly and daily) (monthly) (yearly) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) KP_AP 1932 - Present (3 hourly and daily) (Lists and histograms of geomagnetic disturbance and Solar Sunspots) AE_HV 1957-75, 78-88 (hourly) AE_MIN 1978-881-6;198903;1990-94 (minute) DST 1957 - Present (hourly) PC 1975 - Present (15-minute) AMANAS 1959 - Present (3 hourly and daily) KMKNKS 1983 - Present (3 hourly) . ...

The project of the informational system creation on the problem of evolution of radio galaxies, as a part of the "Big Trio" project aimed on studing of distant radio galaxies, is designed. This system allows a user to operate with simulated curves of spectral energy distributions (SED) to estimate ages and redshifts by photometry data. Authors use SEDs of several models for different types of galaxies. ... The HTTP and e-mail access is organized to this system. ...

... We focus on the mass loss that stars experience along the way to their final stage as white dwarfs Evolution of a Sun-like Star 1. ... 2009): M WD = 0.339 + 0.129M Fit the clusters using both sets of models and a linear IFMR ages 95% Posterior Intervals (M Sun Simulated: Yi Fit: Yi 8 Simulated: Dotter Fit: Yi Simulated: Yi Fit: Dotter ) 6 logAge 4 8.4 8.6 8.8 9.0 9.1 9.2 9.4 9.6 2 2 4 6 8 Sun 2 4 6 8 Sun 2 4 6 8 Sun True Initial Mass (M ) True Initial Mass (M ) True Initial ...

The rotation of the stellar component of galaxy is obtained from the compilation of internal stellar kinematics . The rotation of the gaseous component is given in the parameter vmaxg , and the stellar velocity dispersion in vdis . For disk-like galaxies (eg. mostly disks of spiral), the apparent rotation may be converted into the true (physical) rotation using the inclination given in the parameter incl . HyperLeda . Questions: prugniel@obs.univ-lyon1.fr

... According to modern views on the evolution and origin of stars, most of the stars are members of binary systems. ... After the second explosion, the pairs tend to break up and neutron stars and/or black holes fly apart. High velocities of radio pulsars are apparently largely due to this effect. ... For all possible pairs the probability of trajectory approach at small distances for the epoch, corresponding to the age of the younger pulsar have been evaluated. ... Pulsars J0543+2329 and J0528+2200. ...

... The Radon transform (also known as the Hough transform) is formulated as a family of line integrals through a two-dimensional function. ... The Radon transform provides us with a simple means of computing the FF plane of the autochirplet transform, by using the Wigner distribution, and arriving at a transform space that tells us basically the same information as the chirplet FF-plane, except that we benefit from the greater resolution of the Wigner distribution. ...

In this chapter we will consider two very simple but useful Web agents that I have written on Actor Prolog for my own needs. ... Let us start the Web agent. Fig. ... Start of the Web agent. The Context diagram consists of three blocks: "Logic Programming Sites", "Edit", and "Check". ... Some Web sites that are linked with the logic programming and Prolog are listed in the pulldown list (these addresses are transferred to the "Edit" block from the "Logic Programming Sites" block). ...

... The analysis shows, that asteroid ­ rubble pile loses its fast fragments in no time but the retaining fragments forms a compact structure immersed in dust ­ gas atmosphere, created by interaction of interplanetary medium with dispersed product of collisional evolution of asteroid. By interaction of an asteroid ­ rubble pile with interplanetary medium structures asteroid can increase its brightness on account of blowed up dust simulating phenomenon of distant comet's brightening. ...