2020/04/16 by Adela Kawka, A. Kawka, Jeffrey D. Simpson +9 · 1 citation
Physics and Astronomy · #Amplitude #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Binary number #Brown dwarf #Exoplanet #Gamma-ray bursts and supernovae #Light curve #Orbital inclination #Orbital period #Physics #Radial velocity #Stars #Stellar, planetary, and galactic studies #Supernova #White dwarf #astro-ph.SR
paper · pdf · doi:10.1093/mnrasl/slaa068
Accepted for publication in MNRAS Letters
arxiv created 2020/04/16 · openalex publication_date 2020/04/21 · arxiv updated 2020/05/06 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
ABSTRACT We present the orbit and properties of 2MASS J050051.85−093054.9, establishing it as the closest (d ≈ 71 pc) extremely low-mass white dwarf to the Sun. We find that this star is hydrogen rich with T_\textrm eff≈ 10 500 K, log g ≈ 5.9, and, following evolutionary models, has a mass of ≈0.17 M⊙. Independent analysis of radial velocity and Transiting Exoplanet Survey Satellite(TESS) photometric time series reveals an orbital period of ≈9.5 h. Its high velocity amplitude (K≈ 144~\textrm km \textrm s-1) produces a measurable Doppler beaming effect in the TESSlight curve with an amplitude of 1 mmag. The unseen companion is most likely a faint white dwarf. J0500−0930 belongs to a class of post-common envelope systems that will most likely merge through unstable mass transfer and in specific circumstances lead to Type Ia supernova explosions.