2020/02/29 by Kyohei Kawaguchi, Masaru Shibata, Masaomi Tanaka · 3 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Black hole (networking) #Ejecta #Event (particle physics) #Gamma-ray bursts and supernovae #Kilonova #Mass ratio #Opacity #Pulsars and Gravitational Waves Research #Radiative transfer #Upper and lower bounds #astro-ph.HE #gr-qc
paper · pdf · doi:10.3847/1538-4357/ab8309
published as The Astrophysical Journal, Volume 893, Issue 2, id.153 (2020) · 16 pages, 15 figures
openalex created_date 2020/02/14 · openalex publication_date 2020/04/01 · arxiv created 2020/06/06 · arxiv updated 2020/06/09 · openalex updated_date 2026/08/06
Abstract We derive the upper limit to the ejecta mass of S190814bv, a black hole–neutron star (BH–NS) merger candidate, through radiative transfer simulations for kilonovae with realistic ejecta density profiles, as well as detailed opacity and heating rate models. The limits to the ejecta mass strongly depend on the viewing angle. For the face-on observations (≤45°), the total ejecta mass should be smaller than 0.1 M ⊙ for the average distance of S190814bv ( D = 267 Mpc), while a larger mass is allowed for the edge-on observations. We also derive the conservative upper limits of the dynamical ejecta mass to be 0.02, 0.03, and 0.05 M ⊙ for the viewing angles ≤20°, ≤50°, and ≤90°, respectively. We show that an iz -band observation deeper than 22 mag within 2 days after the gravitational-wave trigger is crucial to detect a kilonova with a total ejecta mass of 0.06 M ⊙ at a distance of D = 300 Mpc. We also show that a strong constraint on the NS mass–radius relation can be obtained if future observations put an upper limit of 0.03 M ⊙ on the dynamical ejecta mass for a BH–NS event with a chirp mass smaller than ≲3 M ⊙ and effective spin larger than ≳0.5.