Gravitational Waves from a Core g Mode in Supernovae as Probes of the High-Density Equation of State

Pia Jakobus; Bernhard Müller; Alexander Heger; Shuai Zha; Jade Powell; Anton Motornenko; Jan Steinheimer; Horst Stöcker

doi:10.1103/PhysRevLett.131.191201

Gravitational Waves from a Core g Mode in Supernovae as Probes of the High-Density Equation of State

Phys Rev Lett. 2023 Nov 10;131(19):191201. doi: 10.1103/PhysRevLett.131.191201.

Authors

Pia Jakobus¹, Bernhard Müller¹, Alexander Heger¹, Shuai Zha², Jade Powell³, Anton Motornenko⁴, Jan Steinheimer⁴, Horst Stöcker⁴

Affiliations

¹ School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia.
² Yunnan Observatories, Chinese Academy of Sciences (CAS), Kunming 650216, China; Key Laboratory for the Structure and Evolution of Celestial Objects, CAS, Kunming 650216, China; and International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, China.
³ Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia.
⁴ Frankfurt Institute for Advanced Studies, Giersch Science Center, Frankfurt am Main, Germany.

PMID: 38000402
DOI: 10.1103/PhysRevLett.131.191201

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 (g mode) below the proto-neutron star convection zone. The mode frequency lies in the range 200≲f≲800 Hz 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.