Gravitational-wave signature of core-collapse supernovae

David Vartanyan; Adam Burrows; Tianshu Wang; Matthew S.B. Coleman; Christopher J. White

doi:https://doi.org/10.1103/PhysRevD.107.103015

Gravitational-wave signature of core-collapse supernovae

David Vartanyan, Adam Burrows, Tianshu Wang, Matthew S.B. Coleman, Christopher J. White

Princeton University

Research output: Contribution to journal › Article › peer-review

Abstract

We calculate the gravitational-wave (GW) signatures of detailed three-dimensional (3D) core-collapse supernova simulations spanning a range of massive stars. Most of the simulations are carried out to times late enough to capture more than 95% of the total GW emission. We find that the f/g-mode and f-mode of protoneutron star oscillations carry away most of the GW power. The f-mode frequency inexorably rises as the protoneutron star (PNS) core shrinks. We demonstrate that the GW emission is excited mostly by accretion plumes onto the PNS that energize modal oscillations and also high-frequency ("haze") emission correlated with the phase of violent accretion. The duration of the major phase of emission varies with exploding progenitor, and there is a strong correlation between the total GW energy radiated and the compactness of the progenitor. Moreover, the total GW emissions vary by as much as 3 orders of magnitude from star to star. For black hole formation, the GW signal tapers off slowly and does not manifest the haze seen for the exploding models. For such failed models, we also witness the emergence of a spiral shock motion that modulates the GW emission at a frequency near ∼100 Hz that slowly increases as the stalled shock sinks. We find significant angular anisotropy of both the high- and low-frequency (memory) GW emissions, though the latter have very little power.

Original language	English (US)
Article number	103015
Journal	Physical review D
Volume	107
Issue number	10
DOIs	https://doi.org/10.1103/PhysRevD.107.103015
State	Published - May 15 2023

ASJC Scopus subject areas

Nuclear and High Energy Physics

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https://doi.org/10.1103/PhysRevD.107.103015

Cite this

@article{7888af75d9794379b545c96201430661,

title = "Gravitational-wave signature of core-collapse supernovae",

abstract = "We calculate the gravitational-wave (GW) signatures of detailed three-dimensional (3D) core-collapse supernova simulations spanning a range of massive stars. Most of the simulations are carried out to times late enough to capture more than 95% of the total GW emission. We find that the f/g-mode and f-mode of protoneutron star oscillations carry away most of the GW power. The f-mode frequency inexorably rises as the protoneutron star (PNS) core shrinks. We demonstrate that the GW emission is excited mostly by accretion plumes onto the PNS that energize modal oscillations and also high-frequency ({"}haze{"}) emission correlated with the phase of violent accretion. The duration of the major phase of emission varies with exploding progenitor, and there is a strong correlation between the total GW energy radiated and the compactness of the progenitor. Moreover, the total GW emissions vary by as much as 3 orders of magnitude from star to star. For black hole formation, the GW signal tapers off slowly and does not manifest the haze seen for the exploding models. For such failed models, we also witness the emergence of a spiral shock motion that modulates the GW emission at a frequency near ∼100 Hz that slowly increases as the stalled shock sinks. We find significant angular anisotropy of both the high- and low-frequency (memory) GW emissions, though the latter have very little power.",

author = "David Vartanyan and Adam Burrows and Tianshu Wang and Coleman, {Matthew S.B.} and White, {Christopher J.}",

note = "Funding Information: We thank Jeremy Goodman, Eliot Quataert, David Radice, Viktoriya Morozova, Hiroki Nagakura, and Benny Tsang for insights and advice during the germination and execution of this project. D. V. acknowledges support from the NASA Hubble Fellowship Program Grant No. HST-HF2-51520. We acknowledge support from the U.S. Department of Energy Office of Science and the Office of Advanced Scientific Computing Research via the Scientific Discovery through Advanced Computing (SciDAC4) program and Grant No. DE-SC0018297 (subaward 00009650), support from the U.S. National Science Foundation (NSF) under Grants No. AST-1714267 and No. PHY-1804048 [the latter via the Max-Planck/Princeton Center (MPPC) for Plasma Physics], and support from NASA under Award No. JWST-GO-01947.011-A. A generous award of computer time was provided by the INCITE program, using resources of the Argonne Leadership Computing Facility, a DOE Office of Science User Facility supported under Contract No. DE-AC02-06CH11357. We also acknowledge access to the Frontera cluster (under Awards No. AST20020 and No. AST21003); this research is part of the Frontera computing project at the Texas Advanced Computing Center under NSF Award No. OAC-1818253. In addition, one earlier simulation was performed on Blue Waters under the sustained-petascale computing project, which was supported by the National Science Foundation (Awards No. OCI-0725070 and No. ACI-1238993) and the state of Illinois. Blue Waters was a joint effort of the University of Illinois at Urbana–Champaign and its National Center for Supercomputing Applications. Finally, the authors acknowledge computational resources provided by the high-performance computer center at Princeton University, which is jointly supported by the Princeton Institute for Computational Science and Engineering (PICSciE) and the Princeton University Office of Information Technology, and our continuing allocation at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC03-76SF00098. Publisher Copyright: {\textcopyright} 2023 American Physical Society.",

year = "2023",

month = may,

day = "15",

doi = "https://doi.org/10.1103/PhysRevD.107.103015",

language = "English (US)",

volume = "107",

journal = "Physical review D",

issn = "2470-0010",

publisher = "American Institute of Physics Publising LLC",

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TY - JOUR

T1 - Gravitational-wave signature of core-collapse supernovae

AU - Vartanyan, David

AU - Burrows, Adam

AU - Wang, Tianshu

AU - Coleman, Matthew S.B.

AU - White, Christopher J.

N1 - Funding Information: We thank Jeremy Goodman, Eliot Quataert, David Radice, Viktoriya Morozova, Hiroki Nagakura, and Benny Tsang for insights and advice during the germination and execution of this project. D. V. acknowledges support from the NASA Hubble Fellowship Program Grant No. HST-HF2-51520. We acknowledge support from the U.S. Department of Energy Office of Science and the Office of Advanced Scientific Computing Research via the Scientific Discovery through Advanced Computing (SciDAC4) program and Grant No. DE-SC0018297 (subaward 00009650), support from the U.S. National Science Foundation (NSF) under Grants No. AST-1714267 and No. PHY-1804048 [the latter via the Max-Planck/Princeton Center (MPPC) for Plasma Physics], and support from NASA under Award No. JWST-GO-01947.011-A. A generous award of computer time was provided by the INCITE program, using resources of the Argonne Leadership Computing Facility, a DOE Office of Science User Facility supported under Contract No. DE-AC02-06CH11357. We also acknowledge access to the Frontera cluster (under Awards No. AST20020 and No. AST21003); this research is part of the Frontera computing project at the Texas Advanced Computing Center under NSF Award No. OAC-1818253. In addition, one earlier simulation was performed on Blue Waters under the sustained-petascale computing project, which was supported by the National Science Foundation (Awards No. OCI-0725070 and No. ACI-1238993) and the state of Illinois. Blue Waters was a joint effort of the University of Illinois at Urbana–Champaign and its National Center for Supercomputing Applications. Finally, the authors acknowledge computational resources provided by the high-performance computer center at Princeton University, which is jointly supported by the Princeton Institute for Computational Science and Engineering (PICSciE) and the Princeton University Office of Information Technology, and our continuing allocation at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC03-76SF00098. Publisher Copyright: © 2023 American Physical Society.

PY - 2023/5/15

Y1 - 2023/5/15

N2 - We calculate the gravitational-wave (GW) signatures of detailed three-dimensional (3D) core-collapse supernova simulations spanning a range of massive stars. Most of the simulations are carried out to times late enough to capture more than 95% of the total GW emission. We find that the f/g-mode and f-mode of protoneutron star oscillations carry away most of the GW power. The f-mode frequency inexorably rises as the protoneutron star (PNS) core shrinks. We demonstrate that the GW emission is excited mostly by accretion plumes onto the PNS that energize modal oscillations and also high-frequency ("haze") emission correlated with the phase of violent accretion. The duration of the major phase of emission varies with exploding progenitor, and there is a strong correlation between the total GW energy radiated and the compactness of the progenitor. Moreover, the total GW emissions vary by as much as 3 orders of magnitude from star to star. For black hole formation, the GW signal tapers off slowly and does not manifest the haze seen for the exploding models. For such failed models, we also witness the emergence of a spiral shock motion that modulates the GW emission at a frequency near ∼100 Hz that slowly increases as the stalled shock sinks. We find significant angular anisotropy of both the high- and low-frequency (memory) GW emissions, though the latter have very little power.

AB - We calculate the gravitational-wave (GW) signatures of detailed three-dimensional (3D) core-collapse supernova simulations spanning a range of massive stars. Most of the simulations are carried out to times late enough to capture more than 95% of the total GW emission. We find that the f/g-mode and f-mode of protoneutron star oscillations carry away most of the GW power. The f-mode frequency inexorably rises as the protoneutron star (PNS) core shrinks. We demonstrate that the GW emission is excited mostly by accretion plumes onto the PNS that energize modal oscillations and also high-frequency ("haze") emission correlated with the phase of violent accretion. The duration of the major phase of emission varies with exploding progenitor, and there is a strong correlation between the total GW energy radiated and the compactness of the progenitor. Moreover, the total GW emissions vary by as much as 3 orders of magnitude from star to star. For black hole formation, the GW signal tapers off slowly and does not manifest the haze seen for the exploding models. For such failed models, we also witness the emergence of a spiral shock motion that modulates the GW emission at a frequency near ∼100 Hz that slowly increases as the stalled shock sinks. We find significant angular anisotropy of both the high- and low-frequency (memory) GW emissions, though the latter have very little power.

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U2 - https://doi.org/10.1103/PhysRevD.107.103015

DO - https://doi.org/10.1103/PhysRevD.107.103015

M3 - Article

SN - 2470-0010

VL - 107

JO - Physical review D

JF - Physical review D

IS - 10

M1 - 103015

ER -

Gravitational-wave signature of core-collapse supernovae

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