Abstract
pc \), with a Gaia G-band magnitude of 12.59. This renders it conducive for continuous observations. The spectral temperature is around 25164 K, in agreement with fitting results K \)) based on a spectral energy distribution. The TESS light curve displays ellipsoidal variation and Doppler beaming without eclipsing features. Through fitting the TESS light curve using the Wilson-Devinney code, we determined the masses for the sdB (\(M_1 = odot \)) and the compact object (\(M_2 = odot \)); the compact object likely is a WD. Furthermore, MESA models suggest that the sdB, with a helium core mass of 0.431 odot \) and a hydrogen envelope mass of \(1.3 odot \), is in the early helium main-sequence phase. The MESA binary evolution shows that the J1710 system is expected to evolve into a double WD system. This means that it is an important source of low-frequency gravitational waves.
Published Version
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