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The Be Star Φ Persei

Published online by Cambridge University Press:  14 August 2015

R. Poeckert*
Affiliation:
Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, Victoria, B.C.

Abstract

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He II (λ 4686) emission has been detected in the spectrum of the binary Be star ɸ Persei. The He II emission has velocity variations which are 180° out of phase with the velocity variations of the primary. The primary velocity curve is determined from the broad He I and H lines, and the Fe II emission lines. The amplitude of the primary velocity curve (K1) is 16 ± 2 km s−1. The amplitude of the He II velocity curve is 121 ± 9 km s−1.

If one assumes that the He II emission arises from the secondary, minimum masses for the primary and secondary are 29 ± 14 M⊙ and 3.8 ± 1.7 M, respectively. We suggest that the secondary is a hot compact star, either the remaining helium core of a once more massive star, or a neutron star. The primary is too cool, Bl IIIe, to have any appreciable He II emission.

Type
IV. Massive Binary Systems
Copyright
Copyright © Reidel 1980