Short Time Variations in the Mass-Loss Rate of Early Type Stars

Details Short Time Variations in the Mass-Loss Rate of Early Type Stars Short Time Variations in the Mass-Loss Rate of Early Type Stars

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984iue..prop.1913w&link_type=abstract

IUE Proposal ID #MLGCW

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Scientific paper

Previous high resolution UV observations of a number of OB and Be stars revealed the sudden appearance and disappearance of narrow, high velocity absorption components in the P-Cygni resonance lines. Detailed analysis of existing data indicates that these features evolve significantly in a matter of hours and previous observations, while providing important insights for some aspects of the mass loss phenomenon, do not have sufficient time resolution to document the behavior of the narrow components or other absorbing material at intermediate velocities in the wind. We propose to carry out frequent monitoring of a primary star and one or two secondary stars which are shown to be currently active, and to obtain high time resolution observations as soon as the UV shell lines or enhanced low velocity absorption are detected. These data are needed to (1) determine the correctness of models which attempt to explain the lack of detection of intermediate velocity UV shell lines, (2) to derive the velocity law for the stellar wind, (3) to construct the ionization structure of the gaseous envelope, (4) to study the brief UV shell phase of Be stars, and (6) to further pin down the time scales for the formation, development, and disappearance of this phenomenon. These investigations will give important clues to the mass loss phenomenon of early type stars.

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