Speaker
Maurice van putten
(Sejong University)
Description
GW observations can probe the central engine of core-collapse supernovae by distinct emission from neutron stars (NS) and black holes (BH). While high-frequency GWs are expected from a NS, relatively low-frequency GWs are expected from a BH-torus system. Scaling of the emission during spin-down of the Kerr BH of mass $M\simeq 2.5M_\odot c^2$ powering GW170817B/GRB170817A predicts an energy output $E_{GW}\sim 3.5\%M_\odot c^2 (M/2.5M_\odot)$ in a descending chirp 0.92 s following GW170817 over the frequency range $f_{GW}=(700−200)(2.5M_\odot/M)$Hz. Accordingly for SN Ib/c events during O4, we expect a horizon distance of $(70 − 190)$ Mpc for the mass-range $M = (3 − 5) M_\odot$ with a probability of detection on par with DNS mergers.
Primary author
Maurice van putten
(Sejong University)
Co-author
Dr
Maryam A Abchouyeh
(Sejong University)
