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Accreting pulsating white dwarfs: Probing heating and rotation

Published online by Cambridge University Press:  09 October 2020

Paula Szkody Open the ORCID record for Paula Szkody [Opens in a new window] ,
Boris Gänsicke ,
Odette Toloza ,
Patrick Godon ,
Edward Sion ,
Stella Kafka ,
Keaton Bell Open the ORCID record for Keaton Bell [Opens in a new window] ,
Zachary Vanderbosch  and
AAVSO observers
Paula Szkody
Affiliation:
Astronomy Department, University of Washington, Seattle, WA 98195 email: [email protected]
Boris Gänsicke
Affiliation:
Department of Physics, University of Warwick, Coventry, CV4 7AL, UK
Odette Toloza
Affiliation:
Department of Physics, University of Warwick, Coventry, CV4 7AL, UK
Patrick Godon
Affiliation:
Astrophysics and Planetary Science, Villanova University, Villanova, PA19085 Rowland Department of Physics & Astronomy, JHU, Baltimore, MD21218
Edward Sion
Affiliation:
Astrophysics and Planetary Science, Villanova University, Villanova, PA19085
Stella Kafka
Affiliation:
AAVSO, 48 Bay State Road, Cambridge, MA02138
Keaton Bell
Affiliation:
Astronomy Department, University of Washington, Seattle, WA 98195 email: [email protected]
Zachary Vanderbosch
Affiliation:
Department of Astronomy, University of Texas, AustinTX78712
AAVSO observers
Affiliation:
Rowland Department of Physics & Astronomy, JHU, Baltimore, MD21218
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Abstract

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The white dwarfs in close, interacting binaries provide a natural laboratory for exploring the effects of heating and angular momentum from the accreting material arriving on the surface from the companion. This study is even more fruitful when it involves a pulsating white dwarf, which allows an exploration of the effects of the accretion on the interior as well as in the atmosphere. The last decade has seen the accomplishment of UV (HST) and optical (ground) studies of several accreting white dwarfs that have undergone a dwarf nova outburst that heated the white dwarf and subsequently returned to its quiescent temperature. The most recent study involves V386 Ser, which underwent its first known outburst in January 2019, after 19 years at quiescence. V386 Ser is unique in that its quiescent pulsation shows a triplet, with spacing indicating a rotation period of 4.8 days, extremely slow for accreting white dwarfs. This paper presents the result of HST ultraviolet spectra obtained 7 months after its outburst that shows the first clear confirmation of shorter period modes being driven following the heating from a dwarf nova outburst.

Keywords

accretiondwarf novaewhite dwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S357: White Dwarfs as Probes of Fundamental Physics: Tracers of Planetary, Stellar and Galactic Evolution , October 2019 , pp. 131 - 133
Copyright
© International Astronomical Union 2020

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