Quasi-Periodic Gravitational-Wave Emission due to the SASI Motion

Kuroda, Takami and Kotake, Kei and Takiwaki, Tomoya. (2017) Quasi-Periodic Gravitational-Wave Emission due to the SASI Motion. In: Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016), 14. 010611.

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Official URL: https://edoc.unibas.ch/59316/

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We present results from fully relativistic three-dimensional core-collapse supernova (CCSN) simulations of a non-rotating 15M⊙ star using three different nuclear equations of state (EoSs). From our simulations, we show that the development of the standing accretion shock instability (SASI) differs significantly depending on the stiffness of nuclear EoS. By evaluating the gravitational-wave (GW) emission, we find a new quasi-periodic GW signature on top of the previously identified high frequency (∼500–1000 Hz) one, which is originated from the g-mode oscillation of the photo-neutron star (PNS) surface. The newly found signal appears in relatively low frequency range from ∼100 to 200 Hz. By analyzing the cycle frequency of the SASI sloshing and spiral modes as well as the mass accretion rate to the emission region, we show that the SASI frequency is correlated with the newly found GW emission frequency. This is because the SASI-induced temporary perturbed mass accretion strikes the PNS surface leading to the quasi-periodic GW emission.
Faculties and Departments:05 Faculty of Science > Departement Physik > Former Organization Units Physics > Theoretische Physik Astrophysik (Thielemann)
UniBasel Contributors:Kuroda, Takami
Item Type:Conference or Workshop Item, refereed
Conference or workshop item Subtype:Conference Paper
Publisher:Japanese Physical Society
Series Name:JPS Conference Proceedings
Note:Publication type according to Uni Basel Research Database: Conference paper
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Last Modified:12 Mar 2018 12:00
Deposited On:12 Mar 2018 08:33

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