Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Abstract
Abstract We analyze the directional dependence of the gravitational wave (GW) emission from 15 3D neutrino radiation hydrodynamic simulations of core-collapse supernovae (CCSNe). Using spin weighted spherical harmonics, we develop a new analytic technique to quantify the evolution of the distribution of GW emission over all angles. We construct a physics-informed toy model that can be used to approximate GW distributions for general ellipsoid-like systems, and use it to provide closed form expressions for the distribution of GWs for different CCSN phases. Using these toy models, we approximate the protoneutron star (PNS) dynamics during multiple CCSN stages and obtain similar GW distributions to simulation outputs. When considering all viewing angles, we apply this new technique to quantify the evolution of preferred directions of GW emission. For nonrotating cases, this dominant viewing angle drifts isotropically throughout the supernova, set by the dynamical timescale of the PNS. For rotating cases, during core bounce and the following tens of milliseconds, the strongest GW signal is observed along the equator. During the accretion phase, comparable—if not stronger—GW amplitudes are generated along the axis of rotation, which can be enhanced by the low T /∣ W ∣ instability. We show two dominant factors influencing themore »
- Publication Date:
- Sponsoring Org.:
- USDOE
- OSTI Identifier:
- 2222931
- Grant/Contract Number:
- SC0015904; 1325 SC0017955; PHY-2309231
- Resource Type:
- Published Article
- Journal Name:
- The Astrophysical Journal
- Additional Journal Information:
- Journal Name: The Astrophysical Journal Journal Volume: 959 Journal Issue: 1; Journal ID: ISSN 0004-637X
- Publisher:
- American Astronomical Society
- Country of Publication:
- United States
- Language:
- English
Citation Formats
Pajkos, Michael A., VanCamp, Steven J., Pan, Kuo-Chuan, Vartanyan, David, Deppe, Nils, and Couch, Sean M. Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae. United States: N. p., 2023.
Web. doi:10.3847/1538-4357/acfca4.
Pajkos, Michael A., VanCamp, Steven J., Pan, Kuo-Chuan, Vartanyan, David, Deppe, Nils, & Couch, Sean M. Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae. United States. https://doi.org/10.3847/1538-4357/acfca4
Pajkos, Michael A., VanCamp, Steven J., Pan, Kuo-Chuan, Vartanyan, David, Deppe, Nils, and Couch, Sean M. Thu .
"Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae". United States. https://doi.org/10.3847/1538-4357/acfca4.
@article{osti_2222931,
title = {Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae},
author = {Pajkos, Michael A. and VanCamp, Steven J. and Pan, Kuo-Chuan and Vartanyan, David and Deppe, Nils and Couch, Sean M.},
abstractNote = {Abstract We analyze the directional dependence of the gravitational wave (GW) emission from 15 3D neutrino radiation hydrodynamic simulations of core-collapse supernovae (CCSNe). Using spin weighted spherical harmonics, we develop a new analytic technique to quantify the evolution of the distribution of GW emission over all angles. We construct a physics-informed toy model that can be used to approximate GW distributions for general ellipsoid-like systems, and use it to provide closed form expressions for the distribution of GWs for different CCSN phases. Using these toy models, we approximate the protoneutron star (PNS) dynamics during multiple CCSN stages and obtain similar GW distributions to simulation outputs. When considering all viewing angles, we apply this new technique to quantify the evolution of preferred directions of GW emission. For nonrotating cases, this dominant viewing angle drifts isotropically throughout the supernova, set by the dynamical timescale of the PNS. For rotating cases, during core bounce and the following tens of milliseconds, the strongest GW signal is observed along the equator. During the accretion phase, comparable—if not stronger—GW amplitudes are generated along the axis of rotation, which can be enhanced by the low T /∣ W ∣ instability. We show two dominant factors influencing the directionality of GW emission are the degree of initial rotation and explosion morphology. Lastly, looking forward, we note the sensitive interplay between GW detector site and supernova orientation, along with its effect on detecting individual polarization modes.},
doi = {10.3847/1538-4357/acfca4},
journal = {The Astrophysical Journal},
number = 1,
volume = 959,
place = {United States},
year = {Thu Nov 30 00:00:00 EST 2023},
month = {Thu Nov 30 00:00:00 EST 2023}
}
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