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- W2765252595 abstract "We report the discovery of the ultracompact hot subdwarf (sdOB) binary OW J074106.0-294811.0 with an orbital period of P$_{rm orb}=44.66279pm1.16times10^{-4}$ min, making it the most compact hot subdwarf binary known. Spectroscopic observations using the VLT, Gemini and Keck telescopes revealed a He-sdOB primary with an intermediate helium abundance, T$_{rm eff}=39 400pm500$ K and log(g)=$5.74pm0.09$. High signal-to-noise ratio lightcurves show strong ellipsoidal modulation resulting in a derived sdOB mass $M_{rm sdOB}=0.23pm0.12$ M$_odot$ with a WD companion ($M_{rm WD}=0.72pm0.17$ M$_odot$). The mass ratio was found to be $q = M_{rm sdOB}/M_{rm WD}=0.32pm0.10$. The derived mass for the He-sdOB is inconsistent with the canonical mass for hot sbudwarfs of $approx0.47$ M$_odot$. To put constraints on the structure and evolutionary history of the sdOB star we compared the derived T$_{rm eff}$, log(g) and sdOB mass to evolutionary tracks of helium stars and helium white dwarfs calculated with Modules for Experiments in Stellar Astrophysics (MESA). We find that the best fitting model is a helium white dwarf with a mass of $0.320$ M$_odot$, which left the common envelope ${approx}1.1$ Myr ago, is consistent with the observations. As a helium white dwarf with a massive white dwarf companion the object will reach contact in 17.6 Myr at an orbital period of 5 min. Depending on the spin-orbit synchronization timescale the object will either merge to form an R CrB star or end up as a stably accreting AM CVn-type system with a helium white dwarf donor." @default.
- W2765252595 created "2017-11-10" @default.
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- W2765252595 date "2017-12-07" @default.
- W2765252595 modified "2023-10-16" @default.
- W2765252595 title "The OmegaWhite Survey for Short-period Variable Stars. V. Discovery of an Ultracompact Hot Subdwarf Binary with a Compact Companion in a 44-minute Orbit" @default.
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- W2765252595 doi "https://doi.org/10.3847/1538-4357/aa9522" @default.
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