... Figure: Massive binary evolutionary track. ... A short glance to this track is sufficient to understand that there are a lot of evolutionary scenario parameters, which affect different stages of the binary evolution. Fortunately, a very limited number of parameters has effect on the compact binary merging rate. ... The most important (and practically unique) parameter changing the galactic binary NS merging rate is the distribution of an additional (kick) velocity imparted to NS at birth. ...

... In this work we present Evolution Strategies (ES) as an efficient method to approximate the initial conditions of the main interacting group of three galaxies in M81. ... In this first attempt we use nonself-gravitating simulations to approximate the initial conditions; even with that restriction our method reproduces the density distribution of the three galaxies with great precision. ... Parameters to produce the simulation in Figure 1 Index 1 is for M81, 2 for M82 and 3 for NGC3077 5. ...

... 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 . ...

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. ...

... The obtained results lead to the following conclusions: a) the heavy element enrichment had taken place in the Galaxy in a few bursts of its activity rether than in a continuons manner; b) these bursts occured during the callapse of the early Galaxy; c) the star formation had been inhibited in the time of the bursts; d) the metal enrichment did not proceed in the periods of star formation, between these bursts of activity. ...

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. ...

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.. ...

... 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. ...

... 0 ) = Z '' '' 0 [(1 \Gamma '')'' 1=2 sin 2 i sin 2!] ... We use the similarity theory to present the non--dimensional period T \ Lambda of the evolution of the parameters '' and i as a product of the independent factors: T \ Lambda = \ Gamma (4=15)(a \ Gamma3 =2 \ Lambda =LD )jL c (c 1 ; c 2 )j. Here LD = Ї k \ Lambda a \ Gamma3 k \ Lambda '' \ Gamma3 =2 k Ї \Gamma1=2 \ Lambda is the non-- dimensional parameter of disturbances similarity dependent on the dynamical characteristics of the ...

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 . ...

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 ) ­ ...

... 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...

Next: Calling Parameters Up: CAL_getRGAFigure Previous: CAL_getRGAFigure Contents . The grating mis-alignment is parameterized with a set of Gaussian functions, whose parameters are stored in the CCF. ... The parameters , , are stored in the CCF. is the number of parameters available in the CCF. is the chromatic magnification that scales the width of the grating mis-alignment distribution as a function of angle of incidence and diffraction angle. ...

... Stellar Evolution is driven entirely by the never ending battle between Pressure and Gravity . As imbalances are reached, the star is driven to find a new Energy source. ... Pressure and gravitational forces are equal, the star is stable and its core is sufficiently hot to fuse Hydrogen into Helium More about main sequence stars . ... The luminosity generated by the core fusion of Helium into Carbon is far greater than the shell luminosity associated with the fusion of Hydrogen into Helium. ...

Next: Power of test Up: Basic principles of Previous: Test statistics . In principle, it is possible to compute a value of the statistic for a single frequency and to test its consistency with a random signal ( ). ... The factor N means that there is an increased probability of accepting a given value of the statistic as consistent with a random signal. ... In the command individual descriptions, we often refer to probability distributions of specific statistics. ...

Model Selection Astro193, March 9 Steps in Hypothesis Testing 1/ Set up 2 possible exclusive hypotheses - two models : M0 ­ null hypothesis ­ formulated to be rejected M1 ­ an alternative hypothesis, research hypothesis 2/ Specify a priori the significance level 3/ Choose a test which: - has the required power - approximates the conditions - finds what is needed to obtain the sampling The model with the largest value provides the best description of the data. ...

... Together, this small group works mostly in the field of Active Galactic Nuclei, exploring their distribution in parameter space (black hole mass, black hole spin, accretion rate) and their evolution in cosmic time. Since the growth and activity of the central black hole, on the one side, and the assembly of the host galaxy, on the other, go very tightly in parallel, the AGN evolution is a convenient window on the more general problem of the formation of cosmic structures. ...

The magnetic mapping is fulfilled by the magnetic field line tracing from the satellite position up to the Ionosphere (stop trace at the altitude 110 km). ... As a rule the Tsyganenko [1987] external magnetic field model and IOPT = 3 (Kp = 2) are used. ... The output file includes the following information: . ... For example the file with name aa9610d1.geo contains the information corresponding to the aposteriory magnetic mapping for INTERBALL Auroral Probe for the first decade of October 1996. ...

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. ...

Chiaki Kobayashi, Ralph Sutherland How galaxies did form and evolution? - to answer this unsolved problem, we are simulating the formation and evolutionary history of galaxies in the Universe, including star formation, supernovae feedback, and chemical enrichment. Comparing the spacial distribution of elements within galaxies with observations, we will examine fundamental physical processes that drive galaxy formation. ... COALA : Universe Galaxy AGN Star Planet ...