Abstract We present a comprehensive photometric and spectroscopic analysis of the Algol-type binary Gaia DR3 1892576067672499328. We identified the system as a spectroscopic binary based on medium-resolution LAMOST spectra. Combined with TESS photometry, we determine an orbital period of P = 2. 47757 (1) days, a low mass ratio of q = 0. 098 ± 0. 002, and an orbital inclination of i = 46. 934^+2. 613-₁. ₁₁ degrees. The orbit is consistent with being circular (e = 0). The binary comprises a M₁ = 1. 817 ^ +0. 106-₀. ₂₀₂ \, M_, R₁ = 1. 265^+0. 121-₀. ₁₆₀\, R_ A-type primary and a Roche-lobe-filling secondary of M₂ = 0. 179 ^ +0. 011-₀. ₀₂₀ \, M_, R₂ = 1. 994 ^ +0. 041-₀. ₀₇₇ \, R_. The double-peak Hα emission line indicates the possible existence of a Keplerian accretion disc. We established a simple standard accretion disc model and modeled the geometric and dynamical properties of the accretion disc. The obtained outer disc radius Rout ≈ 3. 36 ± 0. 43 R⊙ is consistent with the values inferred from the emission velocity of Hα. Systemic velocity variations observed over time suggest the possible presence of a tertiary companion, with a minimum mass of M3 0. 369 ± 0. 024 M⊙. Given the low mass ratio, the secondary may evolve into a proto-helium white dwarf, forming an EL CVn-type system in the future. This system offers valuable insights into accretion dynamics and the formation of binaries.
He et al. (Fri,) studied this question.