Next: A Gravitational Wave Map Previous: Critical Frequencies and Gravitational . In this section we consider the GWB spectrum as such, that is, we study how dimensionless strain metric amplitude h is dependent on frequency. For a sample of N independent binaries emitting GW at a given frequency the net result is . ... are, respectively, effective distance to the sample and effective mass of the binaries (in solar units) producing the GW radiation at the frequency . ...

. 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.

Next: Polarization efficiency: size/shape/orientation effects Up: Optical properties of cosmic Previous: The 2175? feature . To model the interstellar polarization one needs to calculate the forward-transmitted radiation for an ensemble of non-spherical aligned dust grains. ... Let non-polarized stellar radiation passes through a dusty cloud with a homogeneous magnetic field. ... The angle between the line of sight and the magnetic field is ( ). ... where the angle is connected with and ( ). ...

... 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. ...

... 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: This Work Previous: Rotation Periods of ZAMS Stars . ... There are currently several groups involved in the studies of the rotation periods of PMS stars. ... Overall, there are about 100 rotation periods known for PMS stars. ... Furthermore, the stars with periods near 8 days also tend to have infrared excesses which can be interpreted as arising from disks. ... In the first interpretation, the gap occurs because locking mechanism holds stars at a eight day rotation period. ...

ESTIMATIONS OF EFFECTIVE HEIGHT, SIZE AND BRIGHTNESS TEMPERATURE OF SOLAR CYCLOTRON SOURCES A.N. Korzhavin, T.I. Kaltman Sp ecial Astrophysical Observatory of RAS, Saint-Petersburg, Russia arles@mail.ru The mo deling of microwave emission from a sp ot-asso ciated cyclotron source was done to refine the metho d of estimations of effective brightness temp erature, size and height ab ove photosphere in the pro cessing of RATAN-600 observations. ...

Median Twilight Image . all frames normalized by their median before averaging and corrected for 4-port structure) . Median of Normalized Twilight Images at Rotator Angle 0 . Median of Normalized Twilight Images at Random Rotator Angle . Time Frame and Rotator Angle Distribution . B_UT2_2CCD: 134 frames . ... distribution of rotator angles) . U_UT2_2CCD: 106 frames . ... uncorrected median twilight image) . B_UT2: 298 frames . ... U_UT2: 246 frames . ... B_UT3: 266 frames . ...

We studied the radiative transfer in a spherical, two-phase clumpy medium, in which coherent, nonconservative scattering is the dominant opacity source and where the source of photons is situated at the center. ... We examined in detail the cloud mass spectrum, the distribution of optical depths, and the apparent fractal nature of the projected cloud structures. ... The expected reddening is substantially reduced for clumpy media. ...

. Next: Pulsar ages Up: The galactic population of Previous: The observed distribution . љ . Account for selection effects of surveys . , peak of distribution not seen . Derive Observable population . Account for beaming fraction . Total population around 500,000 . љ љ . Figure 19: The observed and derived luminosity functions. From Lyne & Graham-Smith 1990 [ 23 ]. Jon Bell . Thu Dec 19 15:15:11 GMT 1996

... COMPUTER SIMULATION OF RADIOWAVE MULTIPLE SCATTERING EFFECTS IN IONOSPHERE USING MONTE-CARLO METHOD . ... Distribution of reflected radiation on the ground is computed. ... Such influence can be remarkable if the scattering is multiple, i.e. the optical thickness for the scattering process is considerably greater than a unit. ... Radiation energy transfer in the slab is modeled by distribution of some particles carring small portions of radiation energy. ... The isotropic plasma approximation is...

... Tsupko Gravitational Lensing in Plasmic Medium Plasma Physics Reports, 2015, Vol. ... 562­581 The influence of plasma on different effects of gravitational lensing is reviewed. Using the Hamiltonian approach for geometrical optics in a medium in the presence of gravity, an exact formula for the photon deflection angle by a black hole (or another body with a Schwarzschild metric) embedded in plasma with a spherically symmetric density distribution is derived. ...

... Results 3. ... 2004), Escapa (2011): Hamiltonian approach, simplified elastic response. ... PАg. ... Let us recall that assuming a rheological model based in Smith (1974) , Wahr (1979) and IERS (2010) for the elastic/anelastic response of the Earth, the second order harmonic components of the redistribution potential admit a truncated development in complex spherical harmonics in the form Generalized Love Numbers, dependent on: Harmonic order, Excitation frequencies In magnitude, PАg. ...

... Abstract: We present Monte Carlo radiative transfer simulations for spiral galaxies modelled as a stellar disk and a two-phase clumpy dust distribution. ... As a general result, clumpy models are less opaque than the corresponding homogeneous models. ... 0.00 0.15 0.50 0.1 0.5 1.0 2.0 5.0 10.0 0.25 X . ... We have also produced several homogeneous models, to compare to the clumpy models. ... Homogeneous and clumpy models with the same tauV have the same dust mass. ...

... Let be a random deviate which follows a Poissonian probability distribution about the expectation value . Although the Poisson distribution itself is only defined for integer , one can find the following continuous `envelope function' to the Poisson values: . ... where is the gamma function . ... The expectation value of is . ... Equation 5 is used both in the present program and in boxdetect to estimate the null-hypothesis probability distribution of the weighted sum of Poissonian images. ...

... The main field of my investigations is stellar spectrophotometry. As a result of scientific activity of our group spectrophotometric catalog was created including energy distribution data on 900 stars in the range 3200-7600AA and 250 stars in the range 6000-10800AA (Voloshina et al., Spectrophotometry of Bright Stars, ed. I.N.Glushneva, 1982, Moscow, Nauka, in Russian). ...

... We present a computer program for modelling energy flux distribution and light curves of eclipsing binaries from far ultraviolet to infrared regions. The Roche model is assumed. Proximity effects of components (reflection of radiation and surface gravity darkening) are taken into account. ... Figure 1: The surface temperature distribution for Algol A-B system before (upper plot) and after (lower plot) correction for temperature due to the irradiation effect. ...

The above image is a computer simulation of the distribution of mass in a Dark Matter dominated Universe. ... Structure (\eg density enhancements) clearly forms at the intersection of these filaments. ... What is Dark Matter? ... Testing for the presence of dark matter in the solar neighborhood now becomes an accounting problem The possible sources of this mass in the solar neighborhood are 1) luminous stars, 2) interstellar gas, 3) stellar remnants (mostly white dwarfs) and 4) dark matter: . ...

Chair of solid state physics . ... Physics of Semiconductors . ... The electron mean free time. ... The dispersion of electrons and holes. ... The mean values of the velocity and acceleration of the electron, the electrons and holes in a magnetic field (the classical theory), the diamagnetic resonance. ... The energy spectrum of electrons and holes in a magnetic field (quantum theory), the energy spectrum of electrons and holes in a constant electric field (quantum theory), shallow impurity levels. ...

Toward a Quantitative Interpretation of MidIR Spectra of Galaxies B. Nikolic (NRAO), P. Alexander (Cambridge), M. Clemens (Padova), D. Ford (Cambridge), G. Cotter (Oxford), M.S. Longair (Cambridge) The Method Starburst99 + Comprehensive dust model + Simple radiative transfer Allows investigation of the effects of starburst age, metallicity, IMF etc. ... Appropriate for midIR models since only UV/optical photons are important in exciting the emission. ...