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HK: Fachverband Physik der Hadronen und Kerne
HK 31: Nuclear Astrophysics II
HK 31.3: Vortrag
Dienstag, 12. März 2024, 18:15–18:30, HBR 19: C 103
Hyperons in binary neutron star mergers — •Hristijan Kochankovski3, Sebastian Blacker1,2, Andreas Bauswein2,4, Angels Ramos3, and Laura Tolos5 — 1Institut für Kernphysik, Technische Universität Darmstadt, 64289 Darmstadt, Germany — 2GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany — 3epartament de Fisica Quàntica i Astrofisica and Institut de Ciències del Cosmos, Universitat de Barcelona, Mart** i Franquès 1, 08028, Barcelona, Spain — 4Helmholtz Research Academy Hesse for FAIR (HFHF), Campus Darmstadt, 64291 Darmstadt, Germany — 5Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, 08193 Barcelona, Spain
The coalescence of a neutron star binary system is an ideal situation for studying extremely dense and hot matter. It is possible that exotic species like hyperons exist in these extreme conditions. In this talk, I will discuss how the appearance of hyperons affects the equation of state and, in turn, what kind of signatures they can leave in the observables that are measured from astrophysical phenomena. I will pay close attention to the signatures originating from the thermal behavior of hyperons in matter. The thermal pressure significantly decreases when hyperons are present. As a result, in comparison to purely nucleonic EoS models, this effect causes a characteristic increase of the dominant postmerger gravitational-wave frequency by as much as 150 Hz.
Keywords: neutron stars; mergers; hyperons