... 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. ...

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

polimodel -- Produce model linear polarization and position angle images . ... Whether to apply random errors to output polarization and position angle values. seed = "" [integer] . ... This task produces a model linear polarization image and corresponding position angle image from an input image assumed to represent intensity (Stokes I parameter). ... A threshold for the input image can be defined such that polarization and position angle are not computed for input values less than this threshold. ...

Here are some suggestions for subtracting Tiny Tim models from unsaturated WFPC2 PSFs. ... The undersampling of the WPFC2 cameras results in the observed PSF being highly dependent on positioning at the subpixel level. A subsampled model should be generated, shifted to match the proper positioning of the observed PSF, and then rebinned to detector sampling. ... The PSF models will never be perfect matches to the observed ones, and they will likely be too symmetrical. ... Figure 1. ...

. Next: Normal star evolution Up: No Title Previous: Introduction . In the calculations of the evolutionary track both nuclear evolution of the normal star and spin evolution of a magnetized compact object (neutron star (NS) or white dwarf (WD)) are taken into account. Normal star evolution . Initial parameters of compact stars . Sergei B. Popov . Fri Jun 21 19:17:07 MSD 1996

Next: Identification and Analysis of Binary Star Systems using Probability Theory . ... We present a computing code for modelling energy flux distributions, photometric indices and spectral line profiles of (non-)radially pulsating Main-Sequence stars. ... In the case of slowly rotating stars one can use the zero-rotation approximation to describe stellar pulsations. Such a model was used already by Cugier, Dziembowski & Pamyatnykh (1994) to study nonadiabatic observables of Cephei stars. ...

... User Guide ] Task: uvfit Purpose: Fit point sources to a given vis file. ... Key: stokes Normal Stokes/polarisation parameter (e.g. i,q,u,v,ii etc). ... Key: object This gives the object type that uvfit fits for. ... Key: fix This gives a set a flag parameters, one parameter per source. Each parameter consists of a set of letters, which indicate which source parameters of a component are to be held fixed. These source parameters are fixed by the initial estimates given by the `spar' parameter. ...

The Earth's magnetosphere global structure is conditioned by the interaction of the Solar wind and Earth's magnetic field. ... Many various magnetospheric models are available in the NSSDC . ... Fairfield D. H., Average and unusual location of the Earth's magnetopause and bow shock, J. Geophys. ... Stasiewicz K., Polar Cusp Topology and Position as a Function of Interplanetary Magnetic Field and Magnetic Activity: Comparison of a Model with Viking and other Observations, J. Geophys. ...

... While Sfit accepts input from "stdio", it is more natural to save/edit commands in a file (eg "solve_input.sfit") and run the code simply by entering > Sfit solve_input.sfit [linelist] . ... The model grid (3.4MB) produced by Example 1 and a selection of input spectra ( f008 f036 f068 f304 f354 ), together with SFIT output files are also given in this folder . ... The model grid (2.8MB) produced by Example 3 and an input spectrum together with SFIT output files are also given in this folder . ...

... The first EGRET catalog ([ Fichtel et al. 1994b ]) used the galactic diffuse gamma radiation model of Bertsch et al. (1993b). ... For the results presented by Bertsch et al. (1993b), the HI and W radio data were deconvolved by integrating the radio data over a velocity interval determined by the endpoints of each distance interval ( ). ... The Galactic radius limit used in the model has been increased to 30 kpc. ... The CR electron spectrum of Fichtel et al. (1991) was used by Bertsch et al. ...

Russian SHAREABLE DATA CENTER Institute of Solar-Terrestial Physics SB RAS . ... The algorithm and appropriate program for decametric radiosignal propagation conditions prediction for paths from 500 to 9000 km have been developed at ISTP SB on the basis of normal wave method (AltyntsevaB.I,Iliyin N.V., Kurkin V.I. and others //Decameters channel simulation on the base of normal wave method . ... Solar activity indices are chosen automatically from the prediction date from the database . ...