Gravitational-Wave Features from Rapidly Rotating Core-Collapse Supernovae

He-Feng Hsieh^1,2*, Rubén Cabezón³, Li-Ting Ma^2,4,5, Kuo-Chuan Pan^2,4,5,6,7

¹Department of Physics, National Taiwan University, Taipei, Taiwan
²Institute of Astronomy, National Tsing Hua University, Hsinchu, Taiwan
³Center for Scientific Computing - sciCORE, Universität Basel, Basel, Switzerland
⁴Department of Physics, National Tsing Hua University, Hsinchu, Taiwan
⁵Center for Informatics and Computation in Astronomy, National Tsing Hua University, Hsinchu, Taiwan
⁶Center for Theory and Computation, National Tsing Hua University, Hsinchu, Taiwan
⁷Physics Division, National Center for Theoretical Sciences, Taipei, Taiwan

* Presenter:He-Feng Hsieh, email:hfhsieh@phys.ncts.ntu.edu.tw

Detection of gravitational waves (GWs) together with neutrino emissions from nearby core-collapse supernovae (CCSNe) place meaningful constraints on the supernova engines and the nuclear equation of state. In this talk, I will present self-consistent three-dimensional CCSN simulations of a 20 solar-mass rotating progenitor with various initial angular velocities. We identify two strong GW features, with peak frequencies of ∼300 Hz and ∼1.3 kHz in the first 100 ms postbounce. These two features are associated with the m=1 deformation from the proto-neutron star, where the 300 Hz feature is present in models with an initial angular velocity between 1.0 and 4.0 rad/s, while the 1.3 kHz feature is present only in a narrower range, from 1.5 to 3.5 rad/s. In addition to the gravitational bounce signal, the detection (or not) of the 300 Hz and 1.3 kHz GW features could provide additional diagnostics to estimate the initial angular velocity of a collapsing core.

Keywords: Core-collapse supernova, Gravitational wave astronomy, Hydrodynamical simulations