Abstract
Using relativistic supernova simulations of massive progenitor stars with a quark-hadron equation of state (EOS) and a purely hadronic EOS, we identify a distinctive feature in the gravitational-wave signal that originates from a buoyancy-driven mode ( mode) below the proto-neutron star convection zone. The mode frequency lies in the range and decreases with time. As the mode lives in the core of the proto-neutron star, its frequency and power are highly sensitive to the EOS, in particular the sound speed around twice saturation density.
- Received 16 January 2023
- Revised 18 April 2023
- Accepted 29 September 2023
DOI:https://doi.org/10.1103/PhysRevLett.131.191201
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