Stellar winds and magnetic fields in the helium peculiar stars

Journal Article · Tue Sep 01 00:00:00 EDT 1987 · Astron. J.; (United States)

DOI:https://doi.org/10.1086/114511· OSTI ID:5711256

Shore, S N

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, especially 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. 39 references.

• Research Organization: New Mexico Institute of Mining and Technology, Socorro; Observatoire, Meudon, France
• OSTI ID: 5711256
• Journal Information: Astron. J.; (United States), Vol. 94
• Country of Publication: United States
• Language: English

Related Subjects

71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
MAIN SEQUENCE STARS
PLASMA JETS
CHEMICAL COMPOSITION
GAS FLOW
HELIUM
MAGNETIC FIELDS
MASS TRANSFER
RADIOWAVE RADIATION
STELLAR WINDS
ULTRAVIOLET SPECTRA
ELECTROMAGNETIC RADIATION
ELEMENTS
FLUID FLOW
FLUIDS
GASES
NONMETALS
RADIATIONS
RARE GASES
SPECTRA
STARS
STELLAR ACTIVITY
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources