Simulation of variable ultraviolet line blanketing in AP SI stars

Details Simulation of variable ultraviolet line blanketing in AP SI stars Simulation of variable ultraviolet line blanketing in AP SI stars

Nov 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....91..247b&link_type=abstract

Astronomy and Astrophysics, vol. 91, no. 1-2, Nov. 1980, p. 247-250.

Astronomy and Astrophysics

Astronomy

4

A Stars, Hot Stars, Line Spectra, Stellar Atmospheres, Stellar Spectra, Ultraviolet Astronomy, Balmer Series, Magnetic Stars, Silicon, Stellar Spectrophotometry, Ultraviolet Spectra

Scientific paper

The strong absorption which depresses the flux around 1400 A in hot Ap Si stars relative to normal stars has been grossly simulated in NLTE models at Teff equals 13,000 and 15,000 K. The redistribution of the flux begins in the Balmer continuum where it is very strong on the red side of the null wavelength region; it renders the Paschen slope bluer than in the normal stars of the same Teff. For the chosen opacity law, the difference in Teff between normal models and blanketed models of the same Paschen slope is 900 K. The Balmer discontinuity is systematically smaller in the blanketed models than in the comparison models of the same Paschen slope. This result, which agrees with Muthsam (1979), corresponds to the behavior of the Balmer discontinuity analyzed by Gerbaldi (1977).

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