The Mass of the Cepheid Binary V636 Scorpii
- 1 October 1998
- journal article
- research article
- Published by American Astronomical Society in The Astrophysical Journal
- Vol. 505 (2) , 903-909
- https://doi.org/10.1086/306177
Abstract
The mass-luminosity relation for Cepheids depends on the degree of mixing in their main-sequence progenitors. Masses of Cepheids can be inferred by using different aspects of pulsation theory. These methods have in the past led to diverging results, showing that something was wrong in either evolution theory or pulsation theory or both. For some binary Cepheids dynamical masses, which are independent of pulsation and evolution theories, can be determined. V636 Sco is one of a handful of Cepheid binaries whose companions are bright enough in the ultraviolet that orbital radial velocities can be measured. We have here attempted to determine the radial velocity of the companion V636 Sco B to the Cepheid V636 Sco A by means of two Hubble Space Telescope (HST) spectra taken at phases of minimum and maximum Cepheid orbital velocities. The ratio of the orbital velocity of the companion and the Cepheid (which is the inverse of their mass ratio) came out to be 1.25 ± 0.17. V636 Sco B has a spectral type B9.5 V, for which we expect a stellar mass of 2.5 M☉. For the Cepheid we thus determine a mass of 3.1 ± 0.4 M☉, which is surprisingly low. If true, such a low mass would indicate an extremely large amount of excess mixing, which is very unlikely. We discuss the likely possibility that V636 Sco B may itself be a binary with an unseen secondary, in which case the mass derived from the two measurements discussed above is not correct. Although the error limits for the mass of each Cepheid are rather large, the combined mass-luminosity relation for all Cepheids studied by us so far by means of HST spectra indicates excess mixing corresponding to core convective overshoot by 0.25 to about 0.5 pressure scale height in the main-sequence progenitors of the Cepheids.Keywords
This publication has 23 references indexed in Scilit:
- The dynamical mass of the beat cepheid Y carinae and stellar opacities.The Astronomical Journal, 1997
- The Mass of the Classical Cepheid S MuscaeThe Astrophysical Journal, 1997
- Line profiles of Cepheid variables: projection factors and metallic line asymmetriesMonthly Notices of the Royal Astronomical Society, 1994
- Accurate masses and radii of normal starsThe Astronomy and Astrophysics Review, 1991
- The dynamical mass of S MUSCAEThe Astronomical Journal, 1990
- The Cepheid mass problem and Cepheid binariesThe Astrophysical Journal, 1986
- Cepheid companions and the masses of cepheidsSymposium - International Astronomical Union, 1984
- Normal and Abnormal Binary FrequenciesAnnual Review of Astronomy and Astrophysics, 1983
- CNO abundances in Cepheids and supergiants - Theoretical implicationsThe Astrophysical Journal, 1982
- The evolution of intermediate-mass stars from the zero-age main sequence to the base of the asymptotic giant branch as a function of mass and compositionThe Astrophysical Journal Supplement Series, 1981