The circumstellar gas of Sigma Orionis E

Details The circumstellar gas of Sigma Orionis E The circumstellar gas of Sigma Orionis E

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985ap%26ss.116..285n&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 116, no. 2, Nov. 1985, p. 285-297.

Statistics

Computation

26

B Stars, Gas Density, H Alpha Line, Sigma Orionis, Stellar Envelopes, Stellar Magnetic Fields, Axes Of Rotation, Computational Astrophysics, Emission Spectra, Magnetic Dipoles, Periodic Variations, Radiant Flux Density, Stellar Models

Scientific paper

In order to explain the variable Hα emission and the eclipse-like light variation of σ Ori E, the author investigated the circumstellar gas trapped by the stellar magnetic field and corotating with the star. By considering the potential along the magnetic field line, he found that the gas concentrates to a potential minimum. The circumstellar gas forms either two condensations or a disk, depending on the inclination of the magnetic dipole to the stellar rotation axis. The geometrical thickness of the circumstellar disk and the distance from the center of the star to the inner edge of the disk were obtained. The Hα emission line profile at its maximum phase and the amplitude of light variation were calculated by assuming the isothermal gas in LTE.

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