A New Algol-type Binary with an Accretion disk

We present a comprehensive photometric and spectroscopic analysis of the Algol-type binary \textit{Gaia} DR3 1892576067672499328. We identified the system as a spectroscopic binary based on medium-resolution LAMOST spectra. Combined with \textit{TESS} photometry, we determine an orbital period of $P = 2.47757 (1)$ days, a low mass ratio of $q = 0.098 \pm 0.002$, 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 $M_1 = 1.817 ^{ +0.106}_{-0.202} \,M_\odot$, $R_1 = 1.265^{+0.121}_{-0.160}\,R_\odot$ A-type primary and a Roche-lobe-filling secondary of $M_2 = 0.179 ^{ +0.011}_{-0.020} \,M_\odot$, $R_2 = 1.994 ^{ +0.041}_{-0.077} \,R_\odot$. The double-peak H$\alpha$ 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 $R_{\mathrm{out}} \approx 3.36 \pm 0.43\,R_\odot$ is consistent with the values inferred from the emission velocity of H$\alpha$. Systemic velocity variations observed over time suggest the possible presence of a tertiary companion, with a minimum mass of $M_3 > 0.369 \pm 0.024 \,M_\odot$. Given the low mass ratio, the secondary may evolve into a proto-helium white dwarf, forming an \text{EL CVn}-type system in the future. This system offers valuable insights into accretion dynamics and the formation of binaries.