Fluctuations at the blue edge of saturated wind lines in IUE spectra of O-type stars

Details Fluctuations at the blue edge of saturated wind lines in IUE spectra of O-type stars Fluctuations at the blue edge of saturated wind lines in IUE spectra of O-type stars

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993dunw.rept.....o&link_type=abstract

Semiannual Report, 1 Jul. - 31 Dec. 1992 Delaware Univ., Newark. Bartol Research Inst.

Astronomy and Astrophysics

Astronomy

Line Spectra, O Stars, Stellar Spectra, Stellar Winds, Ultraviolet Astronomy, Computer Programs, Hot Stars, Iue, Velocity Distribution

Scientific paper

We examine basic issues involved in synthesizing resonance-line profiles from 1-D, dynamical models of highly structured hot-star winds. Although these models exhibit extensive variations in density as well as velocity, the density scale length is still typically much greater than the Sobolev length. The line transfer is thus treated using a Sobolev approach, as generalized by Rybicki & Hummer (1978) to take proper account of the multiple Sobolev resonances arising from the nonmonotonic velocity field. The resulting reduced-Lambda-matrix equation describing nonlocal coupling of the source function is solved by iteration, and line profiles and then derived from formal solution integration using this source function. The more appropriate methods that instead use either a stationary or a structured, local source function yield qualitatively similar line-profiles, but are found to violate photon conservation by 10 percent or more. The full results suggest that such models may indeed be able to reproduce naturally some of the qualitative properties long noted in observed UV line profiles, such as discrete absorption components in unsaturated lines, or the blue-edge variability in saturated lines. However, these particular models do not yet produce the black absorption troughs commonly observed in saturated lines, and it seems that this and other important discrepancies (e.g., in acceleration time scale of absorption components) may require development of more complete models that include rotation and other 2-D and/or 3-D effects.

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