2021/08/31 by Nicholas Z. Rui, Jim Fuller
Engineering · Physics and Astronomy · #Asteroseismology #Astronomical Observations and Instrumentation #Astronomy #Astrophysics #Galaxy #Gamma-ray bursts and supernovae #Luminosity #Physics #Red giant #Star formation #Stars #Stellar collision #Stellar evolution #Stellar mass #Stellar, planetary, and galactic studies #Surface gravity #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stab2528
13 pages, 6 figures, 1 table, submitted to MNRAS
arxiv created 2021/09/04 · openalex publication_date 2021/09/08 · arxiv updated 2021/09/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
ABSTRACT Stellar mergers are important processes in stellar evolution, dynamics, and transient science. However, it is difficult to identify merger remnant stars because they cannot easily be distinguished from single stars based on their surface properties. We demonstrate that merger remnants can potentially be identified through asteroseismology of red giant stars using measurements of the gravity mode period spacing together with the asteroseismic mass. For mergers that occur after the formation of a degenerate core, remnant stars have overmassive envelopes relative to their cores, which is manifested asteroseismically by a g-mode period spacing smaller than expected for the star’s mass. Remnants of mergers that occur when the primary is still on the main sequence or whose total mass is less than ≈ 2 \rm M_\odot are much harder to distinguish from single stars. Using the red giant asteroseismic catalogues of Vrard, Mosser & Samadi and Yu et al., we identify 24 promising candidates for merger remnant stars. In some cases, merger remnants could also be detectable using only their temperature, luminosity, and asteroseismic mass, a technique that could be applied to a larger population of red giants without a reliable period spacing measurement.