Tomographic Separation of Composite Spectra. III. Ultraviolet Detection of the Hot Companion of phi Persei

Details Tomographic Separation of Composite Spectra. III. Ultraviolet Detection of the Hot Companion of phi Persei Tomographic Separation of Composite Spectra. III. Ultraviolet Detection of the Hot Companion of phi Persei

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...448..878t&link_type=abstract

Astrophysical Journal v.448, p.878

Astronomy and Astrophysics

Astronomy

20

Stars: Binaries: Spectroscopic, Stars: Early-Type, Stars: Emission-Line, Be, Stars: Individual Constellation Name: Phi Persei, Ultraviolet: Stars

Scientific paper

We have used archival lUE high-dispersion UV spectra of the Be binary φ Per and published spectroscopic radial velocity curves to reconstruct the individual primary and secondary spectra using Doppler tomography. The primary's spectrum has rotationally broadened photospheric lines (consistent with a spectral type B0.5 III-Ve) and narrow "shell" lines formed in its circumstellar disk. The recovered secondary spectrum (which contributes only ≍12% of the UV flux) has a very different appearance, with strong emission in C IV λ1550 and many narrow, weak absorption lines (mainly Fe v) similar to those found in the spectra of hot 0-type subdwarfs (in particular the sdO6 star HD 49798). These results strongly support Poeckert's (1981) model in which the secondary is the stripped-down core of a once massive star. Such objects could be the progenitors of unusual supernovae.

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