"Finding" the "missing" solar ultraviolet opacity.

Details "Finding" the "missing" solar ultraviolet opacity. "Finding" the "missing" solar ultraviolet opacity.

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992rmxaa..23..181k&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, Vol. 23, p. 181 - 186

Astronomy and Astrophysics

Astronomy

181

Scientific paper

The author has computed new opacities for model stellar atmospheres and envelopes using a large grant of Cray computer time at the San Diego Supercomputer Center. The opacities include 58,000,000 atomic and diatomic molecular lines. Twelve-step distribution functions are tabulated for 56 temperatures in the range from 2000 K to 200000 K, for 21 log pressures from -2 to 8, for 1212 wavelength intervals from 10 to 10000 nm, for microturbulent velocities 0, 1, 2, 4, and 8 km/s, for scaled solar abundances [+1.0], [+0.5], [+0.3], [+0.2], [+0.1], [+0.0], [-0.1], [-0.2], [-0.3], [-0.5], [-1.0], [-1.5], [-2.0], [-2.5], [-3.0], [-3.5], [-4.0], [-4.5], [-5.0], and [+0.0, no He] (log abundance of elements heavier than helium relative to solar). Rosseland means are also tabulated for each case. The final files for each abundance require two 6250 bpi VAX backup tapes. The author is now distributing tape copies. He hopes to have CD-ROMs available in the near future. A solar photospheric model computed with the new opacities matches the observed energy distribution.

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