... 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 . ...

Еще в разделе: (Показать все результаты (>359) - mavr.sao.ru/ )

... We demonstrate through numerical simulations that model parameters estimated with our technique are essentially bias-free, even when the average number of counts per bin is 1. ... The IW technique avoids such biases by estimating through successive iterations, where for each iteration, j, , and the best-fit parameters are determined by minimization of . ... In our sample, we find that the minimum values and best-fit parameters converge after about 6 iterations. ...

Еще в разделе: (Показать все результаты (>1811) - www.adass.org/ )

• A New Entropy Measure Based on Multiple Resolution and Noise Modeling
• Fitting and Modeling in the ASC Data Analysis Environment
• ADASS 2003 Conference Proceedings

... Focus Model . ... Interface with Tiny Tim . ... The focus model output can be used directly in this field without unit conversion. ... an image illustrating the modeled PSF characteristics . ... links to the output data files, including the fits images of the distorted and undistorted modeled PSF . ... Tiny Tim author Krist provides some personal science examples of earlier WFPC2 Tiny Tim model application, and summarizes the tool's use over 20 years of HST science operations in Krist Burrows (2011)...

Еще в разделе: (Показать все результаты (>15791) - www.stsci.edu/ )

• Model Fitting
• HST Focus Model
• Frontier Fields Lensing Models

... 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. ...

Еще в разделе: (Показать все результаты (>2933) - hea-www.harvard.edu/ )

• Jonathan's ASC documents
• Jonathan's ASC/SDS documents
• Structure of the Spectral Package

... 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) . ...

Еще в разделе: (Показать все результаты (>16728) - www.atnf.csiro.au/ )

• Multi-Plane Models
• Input Parameters to the Self-Calibration Tasks
• Miriad's Calibration Model

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. ...

Еще в разделе: (Показать все результаты (>32) - rp.iszf.irk.ru/ )

Spectropolarimetry and modeling of Galactic Wolf-Rayet star WR156 O LGA M A RY E VA Special Astrophysical Observatory RAS; olga.maryeva@gmail.com For the first time spectropolarimetric observations of Wolf-Rayet star WR156 (WN8h sub-class) were conducted. ... This polarization is, most probably, has an interstellar origin, as its magnitude and orientation are similar to the ones of field stars. ... By its parameters WR156 is similar to other WN8h stars, displaying the line effect. ...

Еще в разделе: (Показать все результаты (>1547) - jet.sao.ru/ )

• http://mavr.sao.ru/hq/ssl/maryeva/Rhodes_poster1.pdf
• http://mavr.sao.ru/hq/balega/PUBL_BAL/PUB_2006/riechers_etal_oh104.9+2.4_eso05.pdf
• Spectral energy distribution

... Towards a Truly Unified Model of AGN . ... The Unified Model holds that the aspect-dependent effects primarily determine the nature of the active galactic nucleus that we observe. ... The full postscript file can be obtained here: . The PASA Latex file can be obtained here: . The postscript file of Fig 1 can be obtained here: . ...

Еще в разделе: (Показать все результаты (>1179) - www.mso.anu.edu.au/ )

• Giant Galaxy String Defies Models of How Universe Evolved

lte-codes . Sterne . ... In 2006, Behara and Jeffery introduced a new file format for the model atmospheres produced by STERNE and used by SPECTRUM and SFIT. ... allow depth-dependent descriptions of composition, and . ... model.lambda_ref <lambda ref > . ... abundance < elem > < abund > . ... structure.abundance < elem > : ( needs N depth ) . ab elem,1 , ab elem,2 , ..., ab elem,Ndepth > . ... structure.tau_ref : ( needs N depth ) . ... structure.opac_ref : ( needs N depth ) . ...

Еще в разделе: (Показать все результаты (>3748) - star.arm.ac.uk/ )

• sfit help file
• Armagh Observatory
• FFIT - Command Syntax

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 . ...

Еще в разделе: (Показать все результаты (>66673) - www.eso.org/ )

• OYSTER home page
• Stellar models
• POLIMODEL (V2.00) --- November00 --- POLIMODEL (V2.00)

... Comparing the periods from the model and P2030 data (.ps) ( .pdf ) . aeroPer.dat...file containing aerostat periods. ... The model was then used to determine the periods that it could generate in pulsar observations. ... rf pulse length: 320 Useconds (this is actually 2 160 usecond pulses that are sequential in time). 7 ipps of 3771., 3504., 3076, 2809., 2903.5, 3289., and 3676. useconds. blanking of the radar signal for 42 degrees of azimuth centered on the observatory direction. ...

Еще в разделе: (Показать все результаты (>3920) - www.naic.edu/ )

• ALFA Receiver Temperature Polynomial Fit
• Modeling the Spectrum
• National Astronomy and Ionosphere Center (Arecibo Observatory)

... The perceptron structure, on the basis of which the database is built, is defined by a number of the input and output parameters and a required accuracy. ... The output perceptron data are the expansion coefficients of the scattering matrix elements in series of the generalized spherical functions. ... As the cluster structure depends on the generation conditions the expansion coefficients were averaged over 5--7 realizations of the clusters (for N . ... is the coefficient number. ...

Еще в разделе: (Показать все результаты (>371) - www.astro.spbu.ru/ )

• Model of clusters
• Database of Optical Properties -- Level: subpage
• Introduction

ON THE IMPACT OF THE GALACTIC ABERRATION ON VLBI-DERIVED PRECESSION MODEL Z.M. MALKIN Pulkovo Observatory Pulkovskoe Ch. ... Corrections to adopted precession rate are usually computed from the linear trends in long-term time series of celestial pole offset (CPO), which are the differences between the measured and the theoretical coordinates of the celestial pole. ... CONCLUSIONS We have estimated the impact of GA on parameters of precession-nutation model derived from VLBI observations. ...

Еще в разделе: (Показать все результаты (>418) - www.gao.spb.ru/ )

• http://www.gao.spb.ru/english/as/j2014/presentations/mosenkov.pdf
• http://www.gao.spb.ru/personal/ivanov/papers/ivanov_miletsky_gao2005.pdf
• http://www.gao.spb.ru/english/personal/malkin/publ/zm14e.pdf

... In this context, (or, in the time domain, l ) are no longer independent variables. They are treated like any of the other parameters: i.e. are assumed to be random variables to be estimated from the observations by fitting a model. ... The MIDAS TSA package contains just one such model, namely Fourier series (SINEFIT/TSA) . ... In the time domain, the most important parameters to be estimated from the data are the correlation length of and time lag between the input signals. ...

Еще в разделе: (Показать все результаты (>1954) - www.sao.ru/ )

• Inter-stellar/galactic Absorption Line Modelling
• Extinction and transformation models
• Edition of the Table Containing the Cloud Model

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 . ...

Еще в разделе: (Показать все результаты (>610) - xray.sai.msu.ru/ )

• Initial binary parameters
• Other parameters of the evolutionary scenario
• Initial parameters of compact stars

... 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. ...

Еще в разделе: (Показать все результаты (>1359) - www.mrao.cam.ac.uk/ )

• Bojan Nikolic -- Talks at the Observatory of Cagliari
• Bojan Nikolic -- Fitting and Comparison of Models of Radio Spectra
• An expanding plasmon model for the radio outbursts of Cir X-1

... Lightcurves of two satellites of Saturn, namely Hyperion (S7) and Phoebe (S9), were modeled using algorithms and programs developed for calculat­ ing the rotational dynamics and constructing theoretical lightcurves of planetary satellites. ... The problem of fitting an observed lightcurve with the model one is solved by varying the initial data and values of the parameters of the problem. ... The value of the MLCE calculated for the deduced initial data and values of the parameters is close to zero....

Еще в разделе: (Показать все результаты (>641) - www.ipa.nw.ru/ )

• http://www.ipa.nw.ru/conference/2002/sovet/PS/GAYAZOV.PS
• Keywords_139
• Keywords_99

. 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.

Еще в разделе: (Показать все результаты (>309) - www.wdcb.ru/ )

• "STP Data" STP Data
• Catalogue 5 of WDC-B

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. ...

Еще в разделе: (Показать все результаты (>107) - selena.sai.msu.ru/ )

• http://selena.sai.msu.ru/Pug/Publications/m44_70_pugacheva.pdf
• Svetlana G. Pugacheva

... config/epatplot.par) | config/epatplot.lyt) | ... SSC-SPR-3052 (scr/ epatplot_mod.f90 ): RAWY set to center value of chip if no RAWY column in input file (as in MOS timing mode) Version 1.6 - 2002-11-13 ( MJF ) ------------------------------- - ( src / epatplot_mod.f90 ): removed obsolete code using hardcoded numbers [as in 1.1.6] Version 1.5 - 2002-11-12 ( MJF ) ------------------------------- - ( src / epatplot_mod.f90 ): call CAL_getPatternFraction*() routines for EPIC MOS - ( ...

Еще в разделе: (Показать все результаты (>13520) - xmm.vilspa.esa.es/ )

• http://xmm.vilspa.esa.es/sas/6.1.0/doc/epatplot/ChangeLog
• http://xmm.vilspa.esa.es/sas/7.1.0/doc/epatplot/ChangeLog
• http://xmm.vilspa.esa.es/calibration/documentation/epic_cal_meetings/200605/VBurwitz.pdf