Line profile variability in winds of OB stars

Details Line profile variability in winds of OB stars Line profile variability in winds of OB stars

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt.........7g&link_type=abstract

Ph.D. Thesis Colorado Univ., Boulder.

Astronomy and Astrophysics

Astronomy

Early Stars, Line Spectra, O Stars, Stellar Spectra, Stellar Winds, Variations, Helium, Ultraviolet Astronomy, Ultraviolet Spectra, Velocity Distribution

Scientific paper

Monitoring of He 2 lambda 4686 in a group of bright Of stars showed that night to night line profile variation in this transition is not limited to the Oef stars, but appears to be common in Of stars. No periodicity in the variation has been detected in any of these stars. Synthetic line profile calculations for He 2 lambda 4686, 3203, and 1640 have shown that the observed line profiles can be reproduced for spherically symmetric, steady winds with monotonic velocity fields, only with models including hypersonic microturbulence, and regions of elevated ionization located in the He 2 line formation zone. The line profile variability can be duplicated only by varying mass flux and ionization simultaneously. UV monitoring of three O stars, delta Ori A, iota Ori A, and 15 Mon has shown that the line profile variability in these stars is non-periodic, and can be attributed to simultaneous variation in mass flux and ionization balance.

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