2021/08/24 by Yuan-Pei Yang
Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Binary number #Brightness #Galaxy #Gamma-ray bursts and supernovae #Globular cluster #Luminosity #Observable #Physics #Population #Pulsars and Gravitational Waves Research #Stars #astro-ph.HE
paper · pdf · doi:10.3847/1538-4357/ac2146
8 pages, 2 figures, accepted for publication in ApJ
arxiv created 2021/08/24 · openalex publication_date 2021/10/01 · arxiv updated 2021/10/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Abstract Fast radio bursts (FRBs) are bright radio transients with short durations and extremely high brightness temperatures, and their physical origins are still unknown. Recently, a repeating source, FRB 20200120E, was found in a globular cluster in the very nearby M81 galaxy. The associated globular cluster has an age of ∼9.13 Gyr, and hosts an old population of stars. In this work, we consider that an FRB source is in a close binary system with a low-mass main-sequence star as its companion. Due to the large burst energy of the FRB, when the companion star stops the FRB, its surface would be heated by the radiation-induced shock, and make reemission. For a binary system with a solar-like companion star and an orbital period of a few days, we find that the reemission is mainly at an optical band, with delays of a few seconds after the FRB. Its luminosity is several times larger than the solar luminosity, and the duration is about hundreds of seconds. Such a transient might be observable in a future multiwavelength follow-up observation for Galactic FRB sources.