VI/78    Theoretical Stellar Flux Spectra for F- to K-type Stars   (Buser+ 1992)

A Library of Theoretical Stellar Flux Spectra. I. Synthetic UBVRI photometry and the metallicity scale for F- to K-type stars BUSER R., KURUCZ R.L. <Astron. Astrophys. 264, 557 (1992)> =1992A&A...264..557B 1992A&A...264..557B
ADC_Keywords: Models, atmosphere ; Stars, late-type ; Description: In conjunction with Kurucz' (1979a,b) models for O to G stars, the present models for F- to K- stars provide an extensive, quasi-homogeneous grid of low-resolution theoretical flux spectra for a significant range in stellar parameters covering mostly of the observed HR diagram. The file bklate.dat contains 242 theoretical model atmosphere flux distributions for late-type stars. These flux distributions were calculated by Buser & Kurucz in 1983-5 using published and unpublished models by Gustafsson and his associates. Please refer to the publication (A&A 264, 447) for a full description of the calculations and a discussion of synthetic UBVRI photometry computed from these models. The models cover the following ranges in the parameter space: ----------------------------------------------------------- number fraction of hydrogen xH =0.9 all models turbulent velocity [km/s] vturb =2.00 234 models vturb =5.00 8 models ----------------------------------------------------------- 3750 ≤ Teff ≤ 6000 (K) 0.75 ≤ log.g ≤ 5.25 (cm/s/s) -3.00 ≤ [Fe/H] ≤ 0.50 (dex) ----------------------------------------------------------- Notice that the model sequence does NOT strictly follow an orderly pattern in parameter space, because the present file was composed from several original files having their individual parameter sequences. The last model (#242) is the solar model. Note that the present file still contains 8 models (out of a total of 242) which have turbulent velocities vturb=5.00 km/s, but whose flux distributions have n o t actually been computed for this value of vturb (=5.00 km/s). Hence, for these models, the flux distributions given in the present file are erroneous and should not be used at all. It is suggested that the user d e l e t e them from the file altogether; for the user's convenience, these models are marked on the accompanying list. References: Kurucz R.L., 1979a, ApJS 40, 1 (CDS Catalogue VI/39) Kurucz R.L., 1979b, in: "Problems of Calibration of Multicolor Photometric Systems", Philip A.G.Davis (ed.), Dudley Obs. Rep. 14, p. 363 File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file bklate.dat 80 24001 The Library of Theoretical Fluxes -------------------------------------------------------------------------------- Structure of File bklate.dat: The data come in a SINGLE ASCII FILE, as follows: * The first block of data gives the wavelengths in nanometers (1 nm = 1.0e-09 m) for the 342 wavelength points on the standard Kurucz grid for which fluxes have been computed. The format is (8f10.1). * The next block of data gives the parameter data for each model listed as follows: +first record: model identification: nmodel,iteff,glog,xscale,vturb,xh where nmodel....running number of model, iteff.....effective temperature, glog......log g (surface gravity), xscale....[A/H] (logarithmic metal abundance), vturb.....turbulent velocity, xh........number fraction of hydrogen. The format is (i5,i6,4f6.2). +Following records: line blanketed fluxes and continuum fluxes: hnu,cont where hnu.......line blanketed emergent surface flux moment in erg/s/cm/cm/Hz, cont......continuum surface flux moment in erg/s/cm/cm/Hz. The format is (7e11.4). Note about the Units: HNU and CONT are expressed as flux moments, and are given in the units ergs/s/cm/cm/Hz (SI: mW/m/m/Hz). Hence FLAMBDA, in units ergs/s/cm/cm/Angstrom, must be calculated from HNU using the equation FLAMBDA=0.4*HNU*c/LAMBDA/LAMBDA, (1) where c=2.997925e17.......is the velocity of light and LAMBDA..............is the wavelength in nanometers (as tabulated at the beginning of the file BKLATE.DAT). The numerical factor of 0.4 (=4*0.1) in equation (1) above comes from the conversion of the flux moment into flux (*4) and from the conversion of flux per nanometer into flux per Angstrom (*0.1). NOTICE however that FLAMBDA still is a surface flux; therefore, calculations of absolute luminosities for the BKLATE models require additional assumptions about the radii of the stars represented by the models. Program to read bklate.dat: Program bklateread c c Roland Buser c Space Telescope Science Institute, Baltimore, U.S.A. c and c University of Basel, Switzerland c c August 1986, update April 1994 c c The following program reads the file BKLATE.DAT of model atmosphere c flux distributions for late-type stars; the program also c generates a listing of parameter values for all the models in c the flux file. c dimension wave(342),hnu(342),cont(342) open(unit=5,name='bklate.dat',status='old') * open(unit=6,name='bklatelist.dat',status='new') write(6,4) read(5,1)wave do 10 i=1,242 read(5,2)nmodel,iteff,glog,xscale,vturb,xh write(6,2)nomdel,iteff,glog,xscale,vturb,xh read(5,3)hnu,cont 10 continue 1 format(8f10.1) 2 format(i5,i6,4f6.2) 3 format(7e11.4) 4 format(1h1,3h #,t8,4hTEFF,t13,5hlog g,t19,5h[A/H],t25,5hvturb, 1t33,2hxH//) close(unit=5) close(unit=6) stop end
(End) Roland Buser [Astron. Inst. Basel] 17-Feb-1995
The document above follows the rules of the Standard Description for Astronomical Catalogues; from this documentation it is possible to generate f77 program to load files into arrays or line by line