학술논문
The First Ultracompact Roche Lobe–Filling Hot Subdwarf Binary.
Document Type
Article
Author
Thomas Kupfer; Evan B. Bauer; Thomas R. Marsh; Jan van Roestel; Eric C. Bellm; Kevin B. Burdge; Michael W. Coughlin; Jim Fuller; JJ Hermes; Lars Bildsten; Shrinivas R. Kulkarni; Thomas A. Prince; Paula Szkody; Vik S. Dhillon; Gabriel Murawski; Rick Burruss; Richard Dekany; Alex Delacroix; Andrew J. Drake; Dmitry A. Duev
Source
Subject
*WHITE dwarf stars
*EARLY stars
*ROCHE equipotentials
*ACCRETION disks
*MASS transfer
*LIGHT curves
*
*
*
*
*
Language
ISSN
0004-637X
Abstract
We report the discovery of the first short-period binary in which a hot subdwarf star (sdOB) filled its Roche lobe and started mass transfer to its companion. The object was discovered as part of a dedicated high-cadence survey of the Galactic plane named the Zwicky Transient Facility and exhibits a period of P = 39.3401(1) minutes, making it the most compact hot subdwarf binary currently known. Spectroscopic observations are consistent with an intermediate He-sdOB star with an effective temperature of = 42,400 ± 300 K and a surface gravity of = 5.77 ± 0.05. A high signal-to-noise ratio GTC+HiPERCAM light curve is dominated by the ellipsoidal deformation of the sdOB star and an eclipse of the sdOB by an accretion disk. We infer a low-mass hot subdwarf donor with a mass MsdOB = 0.337 ± 0.015 and a white dwarf accretor with a mass MWD = 0.545 ± 0.020 . Theoretical binary modeling indicates the hot subdwarf formed during a common envelope phase when a 2.5–2.8 star lost its envelope when crossing the Hertzsprung gap. To match its current , , , and masses, we estimate a post–common envelope period of ≈ 150 minutes and find that the sdOB star is currently undergoing hydrogen shell burning. We estimate that the hot subdwarf will become a white dwarf with a thick helium layer of ≈0.1 , merge with its carbon/oxygen white dwarf companion after ≈17 Myr, and presumably explode as a thermonuclear supernova or form an R CrB star. [ABSTRACT FROM AUTHOR]