2024/10/24 by Xu Ding, Ding, Xu, Kaifan Ji +17
Earth and Planetary Sciences · Mathematics · Physics and Astronomy · #Arithmetic #Astro and Planetary Science #Astronomy #Astrophysics #Binary number #Binary system #Geophysics and Gravity Measurements #Mathematics #Physics #Star (game theory) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.2410.18518
published in arXiv (Cornell University) (Cornell University)
openalex publication_date 2024/10/24 · openalex created_date 2024/11/13 · openalex updated_date 2026/07/28
TIC 157365951 has been classified as a δ Scuti type by the International Variable Star Index (VSX). Through the spectra from Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and its light curve, we further discovered that it is a binary system. This binary system comprises a red dwarf star and a compact star. Through the spectral energy distribution (SED) fitting, we determined the mass of the red dwarf star as M1 = 0.31 ± 0.01 M\odot and its radius as R1 = 0.414 ± 0.004 R\odot. By fitting the double-peaked H\rm α emission, we derived the mass ratio of q = 1.76 ± 0.04 , indicating a compact star mass of M2 = 0.54 ± 0.01 M\odot. Using Phoebe to model the light curve and radial velocity curve for the detached binary system, we obtained a red dwarf star mass of M1 = 0.29 ± 0.02 M\odot, a radius of R1 = 0.39 ± 0.04 R\odot, and a Roche-lobe filling factor of f = 0.995±0.129, which is close to the f=1 expected for a semi-detached system. The Phoebe model gives a compact star mass M2 = 0.53 ± 0.05 M\odot. Constraining the system to be semidetached gives M1 = 0.34 ± 0.02 M\odot, R1 = 0.41 ± 0.01 R\odot, and M2 = 0.62 ± 0.03 M\odot. The consistency of the models is encouraging. The value of the Roche-lobe filling factor suggests that there might be ongoing mass transfer. The compact star mass is as massive as a typical white dwarf.