... 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. ...

... 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) . ...

... HST . ... Lensing Models . ... In order to interpret many of the properties of background lensed galaxies, reliable models of the lensing maps for each cluster are required. Preliminary models for each of the six Frontier Fields clusters have been provided by five independent groups prior to the HST Frontier Fields observing campaign in order to facilitate rapid analysis of the FF data by all members of the community. ... The various groups model the cluster mass distribution in different ways. ...

... readmodel , file _char Read a model file. calcmodel Compute the model data for data sets with non-zero weight. modelchisq () Function. Return reduced of currently loaded data wrt model. binarypos ([ epoch _real [, component _char ]][, lambda = lambda ][, com = com ][, abs = abs ]) Function. ... Use today if no epoch is specified, and use the top hierarchical component if no component is specified. ... Examples: PRINT,MODELK(' A'), PRINT,MODELK(' AB'). modelpx ( component _char ) Function. ...

... Archives . ... In order to understand a learning procedure statistically it is necessary to identify two important aspects: its structural model and its error model. ... Without verification, I saw too often times that simple Gaussian error models are almost always adopted in astronomy. ... Additional but small efforts of the statistically apprehensible quantification of astronomical structure models and associated errors would lead cornucopia of error models beyond simple Gaussian error model. ...

Next: Initial parameters of compact Up: The Model Previous: The Model . To start the calculations, we choose the distributions of initial binary parameters: mass of the primary ZAMS component, ; binary mass ratio, ; and orbital separation, a . ... As for the mass ratio distribution in binaries, the observational information is poor. Meanwhile, from the evolutionary point of view, it is particularly important how different are the initial masses of the components (see, e.g., Trimble 1983). ...

... TEXAS SURVEY: THE PRELIMINARY -35 and stronger than 0.25 Jy is intended to provide accurate (one arc-second rms error) positions, flux densities and structure models for each of the ~70000 sources expected to be listed. ... Average rms position accuracy for point sources is 1" in RA and 0.5" in DEC. ... 1 is the source name in IAU format. ... Thus, (+1,+1) means the second most likely lobe is 51.8" LATER in RA, and 51.8"*sec(z) HIGHER in DEC than the position listed. ...

The Earth's magnetosphere global structure is conditioned by the interaction of the Solar wind and Earth's magnetic field. ... Solar wind (SW) - the region outside BS; . ... Auroral field lines (AUR) region - the funnel-shape cavity restricted by the geocentric distance of the order of 6 RE, between surfaces formed by magnetic field lines emerged from the polar and equatorial OVAL borders; . ... Fairfield D.H., Average and unusual location of the Earth's magnetopause and bow shock, J. Geophys. ...

XMM­Newton CCF Release Page: 1 XMM­Newton CCF Release Note XMM­CCF­REL­267 EPIC MOS response R. D. Saxton, M. Guainazzi 29 July 2010 1 CCF components Name of CCF VALDATE EVALDATE Blocks changed XSCS flag EMOS1 REDIST 0075.CCF 2004­01­01 2020­01­01 PRIMARY NO EMOS2 REDIST 0075.CCF 2004­01­01 2020­01­01 PRIMARY NO 2 Changes In the previous set of EPIC MOS redistribution files, released in December 2005, the end validity date for the last epoch (EMOS1/2 REDIST 0074.CCF) was set to the beginning of 2010. ...

... 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) . ...

... 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