Stellar winds and magnetic fields in the helium peculiar stars

Details Stellar winds and magnetic fields in the helium peculiar stars Stellar winds and magnetic fields in the helium peculiar stars

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987aj.....94..731s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 94, Sept. 1987, p. 731-736.

Astronomy and Astrophysics

Astronomy

47

B Stars, Peculiar Stars, Stellar Magnetic Fields, Stellar Winds, Main Sequence Stars, Radio Jets (Astronomy), Stellar Physics, Ultraviolet Spectra

Scientific paper

This note discusses the consequences of the interaction of radiatively driven mass loss with magnetic fields in upper-main-sequence helium-peculiar stars. The field constrains mass loss to occur in narrow cones above the magnetic poles. These jets can explain the observed behavior of UV resonance lines in the helium-peculiar stars, expecially the sn and helium-rich stars. Suppression of mass outflow at the magnetic equator produces a region in which radiatively driven diffusive mass transport can levitate helium in the hottest stars, producing helium enrichment of the atmosphere. In the cooler stars, the surface becomes progressively more helium poor.

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