... Links given for particles of different shapes allow one to access our graphics illustrating the dependence of various optical properties of model scatterers on their parameters. ... Q ext , Q sca , Q abs , Q bk , albedo, g, Q pr vs x for different m . ... Q ext , Q sca , Q abs , Q bk , albedo, g, Q pr vs x for different m core , m mantle , V core /V total . ... Q ext , Q sca , Q abs , albedo, Q pol vs x for different m, alpha . ...

The dust properties in the Large and Small Magellanic clouds (LMC/SMC) are studied using the HERITAGE Herschel Key Project photometric data in five bands from 100 to 500 m. Three simple models of dust emission were fit to the observations: a single temperature blackbody modified by a power-law emissivity (SMBB), a single temperature blackbody modified by a broken power-law emissivity (BEMBB), and two blackbodies with different temperatures, both modified by the same power-law emissivity (TTMBB). ...

Russian SHAREABLE DATA CENTER Institute of Solar-Terrestial Physics SB RAS . ... Although their determination is based on the scattering process model, independent check-ups by rocket experiments have shown their correctness in experimental applications. ... Ionospheric data analysis, especially during strong disturbances, cannot be without some other kinds of diagnostic tools. ... The lack of data has always been a challange in this case. ...

Next: Initial binary parameters Up: Population synthesis of Previous: Introduction . Monte-Carlo method for statistical simulation of binary evolution was originally proposed by Kornilov & Lipunov (1983a,b) for massive binaries and developed later by Lipunov & Postnov (1987) for low-massive binaries. ... Recently Leitherer & Heckman (1995) have modelled star formation for elliptical and spiral galaxies, taking into consideration only the single stars. ... Initial binary parameters . ...

Next: Stellar models Up: Introduction Previous: Photometry Contents . In a hierarchical stellar system, the separation between two neighboring stars is always much smaller than the separation of this pair from the next companion in the system, be it another pair or a single star. ... They are also numerically easier to handle than non-hierarchical systems, since each pair can be described with the standard orbital parameters, and each star with a small number of physical parameters. ... System . ...

... 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) . ...

... The models provided are: . abs - absorption of x-rays by neutral gas with solar abundances. parameter 1 = . ... parameter 2 = . ... normalization - logarithmic value of the flux density at 1 keV in units of keV cm -2 s -1 keV -1 . ... normalization - logarithmic value of the normalization of the gaussian in units of keV cm -2 s -1 . ... absorption ( params )* model ( params ) . ... A single value for the normalization (i.e., fixed normalization) will force the program to use that value. ...

... 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. ...

THE PARAMETERS INVOLVED IN HAPKE'S MODEL FOR ESTIMATION OF THE COMPOSITION OF THE EJECTA LUNAR TERRAINS. ... In the previous papers we were estimated the surface roughness of the ejecta lunar terrains by means comparison of the local phase function and the average integrated lunar indicatrix. ... The Hapke's theoretical model of the lunar surface reflection. ... For THE PARAMETERS INVOLVED IN HAPKE'S MODEL: S.G. Pugacheva, V.V. Shevchenko a low-albedo lunar surface parameter Bo = 1. ...

... 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...

Figure 1. ... Scattering geometry illustration. ... Maps of scattering angle in the cluster core for standard GCW grains and a Model A nebula (left) and UV-altered GCW grains in the same model (right). ... Degrees of consistency between the scattering angles of different models at different wavelengths. ... Schmidt scattering angles over a wider area. ... Schmidt line-of-sight separations over the same area, derived for two different simplified geometric models. ...

... Previous: Background Fluctuation Analysis from the Multiscale Entropy . ... A new measure of information is defined which is based on noise modeling and incorporates resolution scale. Properties of this measure are discussed. ... Additionally it allows for image noise modeling, and subsequent noise removal. ... Hence information- and entropy-based processing technologies will be necessary for the effective design and implementation of large, future generation, image databases. ...

Next: DIRECT MASSES FOR BXCIR Up: EXTREME HELIUM STARS: PULSATION Previous: PULSATION PROPERTIES . As already indicated, V652Her is an important EHe star because its relatively short pulsation period and large amplitude pulsations allow its overall dimensions to be determined with high precision. ... Saio & Nomoto (1998) made the first successful models for the merger of two carbon-oxygen white dwarfs, and prompted Saio & Jeffery (2000) to attempt models for the merger of two helium white dwarfs. ...

... Paradoxically, signal detection is concerned with fitting models to supposedly random series similarly to mathematical proofs by reductio ad absurdum of the antithesis. ... The quality of the fit is evaluated using a function S of the series , , and . ... A random variable S is characterized by its probability distribution function. ... The special realization of a random series which consists of independent variables of common (gaussian) distribution is called (gaussian) white noise. ...

Irregular phenomena in the Earth Pole oscillation process and temporal variations of geopotential Valery Bondarenko, Vadim Perepelkin s The observed irregular phenomena in the Earth Pole oscillation process are very variety. ... These phenomena indicated in the IERS data are the "abnormal" fluctuation of the Earth Pole coordinates which owing to changing of the geodynamical parameters gives negative result in interpolation and forecast of the first approximation mathematical model. ... Fig. ...

... PropertyBasedTableModel Class Reference . This class provides a table model for just about any QObject. ... init (QList< QObject * > *content, QObject *model, QMap< int, QString > mappings) . ... data (const QModelIndex &item, int role=Qt::DisplayRole) const . ... The init method takes the data to model, as well as an instance of your model class (to use as a model for creating new instances), and a map to know the ordering of the properties to their position (as you want them displayed). ...

... Bojan Nikolic web pages home . ... As an exercise to put through the new InMin library through its paces, I have looked recently at applying Nested Sampling ( Skilling2006 ) algorithm to the fitting of star-formation history as function of redshift. ... The data I used are from Figure 1 of Yuksel08 but I use only the grey data paints, which are just the data originally from Hopkins2006 . ... The next step is to define the function which is the model for the history of the SFR density. ...

XMM ­Newton CCF Release Note XMM ­ CCF ­REL­11 RGS CCD Properties C. Erd October 4, 2000 1 CCF components Name of CCF VALDATE List of Blocks changed CAL VERSION XSCS flag RGS1 ADUCONV 0004 2000 ­02­06T16:50:00 ADUCOEFF, OFFSET GAIN --- NO RGS2 ADUCONV 0005 2000 ­01­25T16:27:00 ADUCOEFF, OFFSET GAIN --- NO RGS1 CTI 0001 1998­01­ 01T00 :00:00 CTI , ... The CCD redistribution function is described with a phenomenological model [1, 3], whose parameters are stored in RGS REDIST. ...

On this page you can compute thermodynamics, opacity and nuclear reaction rates for conditions which exist inside the Sun. ... Logarithmic partial derivative dlogP/dlogT (hi_t) . Logarithmic partial derivative dlogP/dlogRHO (hi_rho) . Logarithmic partial derivative dlogP/dlogX (hi_x) . Logarithmic partial derivative dlogU/dlogT (ksi_t) . ... Input field size does not limit the amount of data entered; you can type or paste thousands of lines (10,000 lines tested with output size over 5MB). ...

... We find a transition of LBV star from the LBV instability strip to the region of classical WN for the first time. ... Numerical modeling of the atmospheres of these objects are very important for understanding the evolutionary relationship WR and LBV stars, as well as of the physical causes of LBVs variability. We studied spectra of two very luminous stars in the M33 galaxy - LBV V532 and late WN star FSZ35. ... Bottom: The spectrum of FSZ35 with the final model . ...