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V1187 Herculis: A Red Novae progenitor, and the most extreme mass ratio binary known

Published online by Cambridge University Press:  30 December 2019

Ronald G. Samec ,
Heather Chamberlain ,
Daniel Caton ,
Russell Robb  and
Danny R. Faulkner
Ronald G. Samec
Affiliation:
Pisgah Astronomical Research Institute email: [email protected]
Heather Chamberlain
Affiliation:
Pisgah Astronomical Research Institute email: [email protected]
Daniel Caton
Affiliation:
Dark Sky Observatory, Appalachian State University
Russell Robb
Affiliation:
University of Victoria
Danny R. Faulkner
Affiliation:
Johnson Observatory
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Abstract

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Complete BVRCIC light curves of V1187 Her were obtained in May 2017 at the Dark Sky Observatory in North Carolina with the 0.81-m reflector of Appalachian State University. Earlier, spectra were taken at the Dominion Astrophysical Observatory with the 1.8-m telescope. The spectral type was found to be F8±1 V (6250 K), so the binary is of solar-type. V1187 Her was previously identified as a low amplitude (V < 0.2 mag), short period, overcontact eclipsing binary (EW) with a period of 0.310726 d. Strikingly, despite its low amplitude, the early light curves show total eclipses (eclipse duration ≍31.5 minutes), which is a characteristic of an extreme mass ratio binary. A period study covering 11 years reveals a continuous period decrease dP/dt=–4.7×10–9 d yr–1. The multi-band Wilson-Devinney light curve solution gives a fill-out of 79% and a mass ratio of only 0.0440±0.0001. There is a cool spot region on the secondary component, which is 400 K hotter than the primary. The inclination is only 66.85±0.05 despite the system’s total eclipses.

Keywords

Stars:binaries: eclipsingstars: individual: V1187 Her
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S346: High-mass X-ray Binaries: Illuminating the Passage from Massive Binaries to Merging Compact Objects , August 2018 , pp. 288 - 293
Copyright
© International Astronomical Union 2019 

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