2023/07/02 by Alekzander Kosakowski, Kosakowski, Alekzander, Thomas Kupfer +4
Physics and Astronomy · #Astrophysical Phenomena and Observations #FOS: Physical sciences #Gamma-ray bursts and supernovae #High Energy Astrophysical Phenomena (astro-ph.HE) #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.2307.00645
openalex publication_date 2023/07/02 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/01
We present an analysis of new and archival data to the 20.506-minute LISA verification binary J052610.42+593445.32 (J0526+5934). Our joint spectroscopic and photometric analysis finds that the binary contains an unseen M1=0.89±0.11~\rm M_\odot CO-core white dwarf primary with an M2=0.38±0.07~\rm M_\odot post-core-burning subdwarf, or low-mass white dwarf, companion. Given the short orbital period and relatively large total binary mass, we find that LISA will detect this binary with signal-to-noise ratio 44 after 4 years of observations. J0526+5934 is expected to merge within 1.8±0.3~\rm Myr and likely result in a \rm D6 scenario Type Ia supernova or form a He-rich star which will evolve into a massive single white dwarf.