Spectral flux from low-density photospheres - Numerical results

Details Spectral flux from low-density photospheres - Numerical results Spectral flux from low-density photospheres - Numerical results

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...301..220h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 301, Feb. 1, 1986, p. 220-229.

Statistics

Computation

33

Photosphere, Radiative Transfer, Stellar Atmospheres, Stellar Spectra, Supernovae, Atmospheric Scattering, B Stars, Computational Astrophysics, Continuous Spectra, Hubble Constant, Opacity, Stellar Temperature

Scientific paper

Radiative transfer through sharp, quasi-static atmospheres whose opacity is dominated by hydrogen is considered at densities low enough that scattering usually dominates absorption and radiative excitations usually dominate collisional excitations. Numerical results for the continuum spectral flux are obtained for effective temperatures T(e) = 6000-16,000 K and scale heights Delta-R = 10 to the 10th - 10 to the 14th cm. Spectra are significantly different than if LTE level populations were assumed. Comparison with observations of the Type II supernova 1980k tends to increase the value of the Hubble constant previously obtained by the Baade (1926) method.

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