The first ultracompact Roche lobe–filling hot subdwarf binary
Kupfer, Thomas; Bauer, Evan B.; Marsh, Thomas R.; Roestel, Jan van; Bellm, Eric C.; Burdge, Kevin B.; Coughlin, Michael W.; Fuller, Jim; Hermes, J.J.; Bildsten, Lars; Kulkarni, Shrinivas R.; Prince, Thomas A.; Szkody, Paula; Dhillon, Vik S.; Murawski, Gabriel; Burruss, Rick; Dekany, Richard; Delacroix, Alex; Drake, Andrew J.; Duev, Dmitry A.; Feeney, Michael; Graham, Matthew J.; Kaplan, David L.; Laher, Russ R.; Littlefair, S.P.; Masci, Frank J.; Riddle, Reed; Rusholme, Ben; Serabyn, Eugene; Smith, Roger M.; Shupe, David L.; Soumagnac, Maayane T.
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 T_eff = 42,400 ± 300 K and a surface gravity of log(g) = 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 M_⊙ and a white dwarf accretor with a mass MWD = 0.545 ± 0.020 M_⊙. Theoretical binary modeling indicates the hot subdwarf formed during a common envelope phase when a 2.5–2.8 M_⊙ star lost its envelope when crossing the Hertzsprung gap. To match its current P_orb, T_eff, log(g), and masses, we estimate a post–common envelope period of P_orb ≈ 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 M_⊙, merge with its carbon/oxygen white dwarf companion after ≈17 Myr, and presumably explode as a thermonuclear supernova or form an R CrB star.
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