General-relativistic simulations of three-dimensional core-collapse supernovae

Christian D. Ott, Ernazar Abdikamalov, Philipp Mösta, Roland Haas, Steve Drasco, Evan P. O'Connor, Christian Reisswig, Casey A. Meakin, Erik Schnetter

Research output: Contribution to journalArticle

110 Citations (Scopus)

Abstract

We study the three-dimensional (3D) hydrodynamics of the post-core-bounce phase of the collapse of a 27 M· star and pay special attention to the development of the standing accretion shock instability (SASI) and neutrino-driven convection. To this end, we perform 3D general-relativistic simulations with a three-species neutrino leakage scheme. The leakage scheme captures the essential aspects of neutrino cooling, heating, and lepton number exchange as predicted by radiation-hydrodynamics simulations. The 27 M · progenitor was studied in 2D by Müller et al., who observed strong growth of the SASI while neutrino-driven convection was suppressed. In our 3D simulations, neutrino-driven convection grows from numerical perturbations imposed by our Cartesian grid. It becomes the dominant instability and leads to large-scale non-oscillatory deformations of the shock front. These will result in strongly aspherical explosions without the need for large-scale SASI shock oscillations. Low-ℓ-mode SASI oscillations are present in our models, but saturate at small amplitudes that decrease with increasing neutrino heating and vigor of convection. Our results, in agreement with simpler 3D Newtonian simulations, suggest that once neutrino-driven convection is started, it is likely to become the dominant instability in 3D. Whether it is the primary instability after bounce will ultimately depend on the physical seed perturbations present in the cores of massive stars. The gravitational wave signal, which we extract and analyze for the first time from 3D general-relativistic models, will serve as an observational probe of the postbounce dynamics and, in combination with neutrinos, may allow us to determine the primary hydrodynamic instability.

Original languageEnglish
Article number115
JournalAstrophysical Journal
Volume768
Issue number2
DOIs
Publication statusPublished - May 10 2013
Externally publishedYes

Fingerprint

supernovae
neutrinos
convection
shock
simulation
accretion
hydrodynamics
leakage
oscillation
perturbation
heating
oscillations
M stars
shock fronts
vigor
massive stars
gravitational waves
explosions
leptons
explosion

Keywords

  • gravitation
  • gravitational waves
  • hydrodynamics
  • neutrinos
  • supernovae: general

ASJC Scopus subject areas

  • Nuclear and High Energy Physics
  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Ott, C. D., Abdikamalov, E., Mösta, P., Haas, R., Drasco, S., O'Connor, E. P., ... Schnetter, E. (2013). General-relativistic simulations of three-dimensional core-collapse supernovae. Astrophysical Journal, 768(2), [115]. https://doi.org/10.1088/0004-637X/768/2/115

General-relativistic simulations of three-dimensional core-collapse supernovae. / Ott, Christian D.; Abdikamalov, Ernazar; Mösta, Philipp; Haas, Roland; Drasco, Steve; O'Connor, Evan P.; Reisswig, Christian; Meakin, Casey A.; Schnetter, Erik.

In: Astrophysical Journal, Vol. 768, No. 2, 115, 10.05.2013.

Research output: Contribution to journalArticle

Ott, CD, Abdikamalov, E, Mösta, P, Haas, R, Drasco, S, O'Connor, EP, Reisswig, C, Meakin, CA & Schnetter, E 2013, 'General-relativistic simulations of three-dimensional core-collapse supernovae', Astrophysical Journal, vol. 768, no. 2, 115. https://doi.org/10.1088/0004-637X/768/2/115
Ott, Christian D. ; Abdikamalov, Ernazar ; Mösta, Philipp ; Haas, Roland ; Drasco, Steve ; O'Connor, Evan P. ; Reisswig, Christian ; Meakin, Casey A. ; Schnetter, Erik. / General-relativistic simulations of three-dimensional core-collapse supernovae. In: Astrophysical Journal. 2013 ; Vol. 768, No. 2.
@article{0c55b2fd3879460a97db98871776e049,
title = "General-relativistic simulations of three-dimensional core-collapse supernovae",
abstract = "We study the three-dimensional (3D) hydrodynamics of the post-core-bounce phase of the collapse of a 27 M· star and pay special attention to the development of the standing accretion shock instability (SASI) and neutrino-driven convection. To this end, we perform 3D general-relativistic simulations with a three-species neutrino leakage scheme. The leakage scheme captures the essential aspects of neutrino cooling, heating, and lepton number exchange as predicted by radiation-hydrodynamics simulations. The 27 M · progenitor was studied in 2D by M{\"u}ller et al., who observed strong growth of the SASI while neutrino-driven convection was suppressed. In our 3D simulations, neutrino-driven convection grows from numerical perturbations imposed by our Cartesian grid. It becomes the dominant instability and leads to large-scale non-oscillatory deformations of the shock front. These will result in strongly aspherical explosions without the need for large-scale SASI shock oscillations. Low-ℓ-mode SASI oscillations are present in our models, but saturate at small amplitudes that decrease with increasing neutrino heating and vigor of convection. Our results, in agreement with simpler 3D Newtonian simulations, suggest that once neutrino-driven convection is started, it is likely to become the dominant instability in 3D. Whether it is the primary instability after bounce will ultimately depend on the physical seed perturbations present in the cores of massive stars. The gravitational wave signal, which we extract and analyze for the first time from 3D general-relativistic models, will serve as an observational probe of the postbounce dynamics and, in combination with neutrinos, may allow us to determine the primary hydrodynamic instability.",
keywords = "gravitation, gravitational waves, hydrodynamics, neutrinos, supernovae: general",
author = "Ott, {Christian D.} and Ernazar Abdikamalov and Philipp M{\"o}sta and Roland Haas and Steve Drasco and O'Connor, {Evan P.} and Christian Reisswig and Meakin, {Casey A.} and Erik Schnetter",
year = "2013",
month = "5",
day = "10",
doi = "10.1088/0004-637X/768/2/115",
language = "English",
volume = "768",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - General-relativistic simulations of three-dimensional core-collapse supernovae

AU - Ott, Christian D.

AU - Abdikamalov, Ernazar

AU - Mösta, Philipp

AU - Haas, Roland

AU - Drasco, Steve

AU - O'Connor, Evan P.

AU - Reisswig, Christian

AU - Meakin, Casey A.

AU - Schnetter, Erik

PY - 2013/5/10

Y1 - 2013/5/10

N2 - We study the three-dimensional (3D) hydrodynamics of the post-core-bounce phase of the collapse of a 27 M· star and pay special attention to the development of the standing accretion shock instability (SASI) and neutrino-driven convection. To this end, we perform 3D general-relativistic simulations with a three-species neutrino leakage scheme. The leakage scheme captures the essential aspects of neutrino cooling, heating, and lepton number exchange as predicted by radiation-hydrodynamics simulations. The 27 M · progenitor was studied in 2D by Müller et al., who observed strong growth of the SASI while neutrino-driven convection was suppressed. In our 3D simulations, neutrino-driven convection grows from numerical perturbations imposed by our Cartesian grid. It becomes the dominant instability and leads to large-scale non-oscillatory deformations of the shock front. These will result in strongly aspherical explosions without the need for large-scale SASI shock oscillations. Low-ℓ-mode SASI oscillations are present in our models, but saturate at small amplitudes that decrease with increasing neutrino heating and vigor of convection. Our results, in agreement with simpler 3D Newtonian simulations, suggest that once neutrino-driven convection is started, it is likely to become the dominant instability in 3D. Whether it is the primary instability after bounce will ultimately depend on the physical seed perturbations present in the cores of massive stars. The gravitational wave signal, which we extract and analyze for the first time from 3D general-relativistic models, will serve as an observational probe of the postbounce dynamics and, in combination with neutrinos, may allow us to determine the primary hydrodynamic instability.

AB - We study the three-dimensional (3D) hydrodynamics of the post-core-bounce phase of the collapse of a 27 M· star and pay special attention to the development of the standing accretion shock instability (SASI) and neutrino-driven convection. To this end, we perform 3D general-relativistic simulations with a three-species neutrino leakage scheme. The leakage scheme captures the essential aspects of neutrino cooling, heating, and lepton number exchange as predicted by radiation-hydrodynamics simulations. The 27 M · progenitor was studied in 2D by Müller et al., who observed strong growth of the SASI while neutrino-driven convection was suppressed. In our 3D simulations, neutrino-driven convection grows from numerical perturbations imposed by our Cartesian grid. It becomes the dominant instability and leads to large-scale non-oscillatory deformations of the shock front. These will result in strongly aspherical explosions without the need for large-scale SASI shock oscillations. Low-ℓ-mode SASI oscillations are present in our models, but saturate at small amplitudes that decrease with increasing neutrino heating and vigor of convection. Our results, in agreement with simpler 3D Newtonian simulations, suggest that once neutrino-driven convection is started, it is likely to become the dominant instability in 3D. Whether it is the primary instability after bounce will ultimately depend on the physical seed perturbations present in the cores of massive stars. The gravitational wave signal, which we extract and analyze for the first time from 3D general-relativistic models, will serve as an observational probe of the postbounce dynamics and, in combination with neutrinos, may allow us to determine the primary hydrodynamic instability.

KW - gravitation

KW - gravitational waves

KW - hydrodynamics

KW - neutrinos

KW - supernovae: general

UR - http://www.scopus.com/inward/record.url?scp=84877061060&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84877061060&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/768/2/115

DO - 10.1088/0004-637X/768/2/115

M3 - Article

VL - 768

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 115

ER -