Helium inhomogeneities in main-sequence magnetic stars

Details Helium inhomogeneities in main-sequence magnetic stars Helium inhomogeneities in main-sequence magnetic stars

Dec 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...252..618v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 252, no. 2, Dec. 1991, p. 618-624.

Astronomy and Astrophysics

Astrophysics

54

Helium, Magnetic Stars, Main Sequence Stars, Stellar Composition, Stellar Mass Ejection, Stellar Oscillations, Abundance, Iue, Photosphere, Stellar Magnetic Fields, Stellar Winds

Scientific paper

Helium abundance variations are computed in models of main-sequence magnetic stars with masses in the range 1.6-5 solar mass (Teff = 8,000-19,000 K). To represent a predominantly dipolar magnetic field, regions in the stars are schematically designated either polar, with vertical magnetic fields, or equatorial, with horizontal fields. A stellar wind is supposed to exist at the magnetic poles. The mass-loss rate is varied as a free parameter in the computations. Under these conditions, helium is underabundant at the magnetic equators, while it can accumulate at the poles in the region of the first ionization of helium. The accumulation occurs if the mass-loss rate is of the order of that caused by the solar wind. The helium peak is visible in the atmospheres of the hottest stars, which can account for the observed He-rich stars. It lies below the photosphere and should not be visible in the coolest stars; but it can help to excite the pulsations of rapidly oscillating Ap stars by the Kappa mechanism.

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