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WM-basic Fluxes Support Method Remarks

	Fluxes and Synthetic Spectra of Hot Stars 0.5 Solar Metallicity

	Download of the Complete Model File: All models in a self-extracting archive (20-December-99, 590KB) Models-0.5 Archive by HTTP Models: Model Teff log g R dM/dt vinf data preview (K) (cgs) (Rsun ) (Msun/yr) (km/s) dwarfs d30 (plot) 30000 4.0 8.0 5.5 × 10-8 1505. d35 (plot) 35000 4.0 9.0 1.7 × 10-7 1970. d40 (plot) 40000 4.0 10.0 4.9 × 10-7 2466. d45 (plot) 45000 4.0 11.0 1.3 × 10-6 2843. d50 (plot) 50000 4.0 12.0 2.9 × 10-6 3205. supergiants s30 (plot) 30000 3.0 27.0 1.9 × 10-6 1497. s35 (plot) 35000 3.2 24.0 3.3 × 10-6 1683. s40 (plot) 40000 3.4 21.0 5.2 × 10-6 1795. s45 (plot) 45000 3.6 18.0 6.5 × 10-6 2098. s50 (plot) 50000 3.8 15.0 7.0 × 10-6 2384. top Overview: All models use Z = 0.5 Zsolar and Y = nHe/nH = 0.1. Simulated shock emission has been neglected, and spectral lines have been calculated from 160 Å to about 2000 Å; outside of this range just continuum opacities have been considered. Data: All files contain a short header and 4 columns of data. The header lines are flagged with a "#'' for quick plotting with gnuplot (which treats those lines as comments). The columns are: Wavelength in Angstroms (Ångströms). Eddington flux Hnu (note: nu, not lambda) in erg/cm2/s/Hz. Continuum flux (same units). Normalized spectrum (second column divided by third column). The flux has been normalized to correspond to the effective temperature at the photospheric radius. top
	Last updated January 11, 2000