A New Algol-type Binary with an Accretion disc

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.