The polarized dust shell around Alpha Orionis. II - The silicon fractional condensation, mass-loss rate and grain radius

Details The polarized dust shell around Alpha Orionis. II - The silicon fractional condensation, mass-loss rate and grain radius The polarized dust shell around Alpha Orionis. II - The silicon fractional condensation, mass-loss rate and grain radius

Nov 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...168..217m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 168, no. 1-2, Nov. 1986, p. 217-224.

Astronomy and Astrophysics

Astrophysics

16

Grain Size, Polarization Characteristics, Silicon, Stellar Envelopes, Stellar Mass Ejection, Supergiant Stars, Condensing, Mie Scattering, Stellar Luminosity, Stellar Models, Ubv Spectra

Scientific paper

Within reasonable assumptions, constraints are placed on the fraction of Si in grains, the mass-loss rate of the star, and the grain size, by modeling with the Mie theory the dust scattering polarized light measured in UBV by Borgne (1986) around Alpha Orionis. By considering a unique grain radius, a lower limit of the product of the fractional condensation of silicon with the mass-loss rate is derived which is about 5 x 10 to the -8th solar masses/yr, corresponding to the most efficient size for polarized scattering, 0.08 microns. The present data are consistent with Mathis et al.'s (1977) a exp-3.5 law, and they strengthen the case for a small fraction of Si locked in grains with a total mass-loss rate of 3 x 10 to the -6th solar masses/yr.

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