The Seat of Stellar-Wind Instabilities: CYCLE4 Medium

Details The Seat of Stellar-Wind Instabilities: CYCLE4 Medium The Seat of Stellar-Wind Instabilities: CYCLE4 Medium

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994hst..prop.5315h&link_type=abstract

HST Proposal ID #5315

Computer Science

Hst Proposal Id #5315 Hot Stars Massive Stars

Scientific paper

IUE observations have established that high-velocity variability in UV P-Cygni profiles is a fundamental property of radiatively-driven winds, and that this variability is a signature of the line-driven instability. It is unclear, however, whether the variability is completely intrinsic to the flow, or if it requires a perturbing `seed' from the low-velocity regime. IUE observations lack adequate signal/noise to address this problem; existing HST results are ambiguous. We propose to obtain high-quality time-series HRS spectroscopy of 68 Cygni, a star extensively observed with IUE, in order to provide an empirical answer to this question. These data will distinguish between low-velocity, mechanically-driven instabilities and intrinsic, radiatively-driven instabilities, and will define the interaction of the two regimes. The results will, in turn, have wider implications for the applicability of steady-state wind models, and will provide basic constraints on our radiation hydro code.

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