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Absorption line profiles in a companion spectrum of a mass losing cool supergiant
| Content Provider | NASA Technical Reports Server (NTRS) |
|---|---|
| Author | Boehm-Vitense, Erika Rodrigues, Liliya L. |
| Copyright Year | 1990 |
| Description | Cool star winds can best be observed in resonance absorption lines seen in the spectrum of a hot companion, due to the wind passing in front of the blue star. We calculated absorption line profiles that would be seen in the ultraviolet part of the blue companion spectrum. Line profiles are derived for different radial dependences of the cool star wind and for different orbital phases of the binary. Bowen and Wilson find theoretically that stellar pulsations drive mass loss. We therefore apply our calculations to the Cepheid binary S Muscae which has a B5V companion. We find an upper limit for the Cepheid mass loss of M less than or equal to 7 x 10(exp -10) solar mass per year provided that the stellar wind of the companion does not influence the Cepheid wind at large distances. |
| File Size | 1237538 |
| Page Count | 45 |
| File Format | |
| Alternate Webpage(s) | http://archive.org/details/NASA_NTRS_Archive_19920024986 |
| Archival Resource Key | ark:/13960/t1wd8rz8t |
| Language | English |
| Publisher Date | 1990-01-01 |
| Access Restriction | Open |
| Subject Keyword | Astronomy Stellar Spectra Stellar Winds Line Shape Cool Stars Ultraviolet Spectra Blue Stars Unsteady Flow Stellar Envelopes Stellar Mass Supergiant Stars Stellar Spectrophotometry Absorption Spectra Companion Stars Line Spectra Cepheid Variables Mass Flow Resonance Lines Ntrs Nasa Technical Reports Server (ntrs) Nasa Technical Reports Server Aerodynamics Aircraft Aerospace Engineering Aerospace Aeronautic Space Science |
| Content Type | Text |
| Resource Type | Technical Report |
