Users/Home/repos/gr21posterfedrow/affinityd/7 21 after ...future/wp-content/... · J.M.Fedrow,...

J. M. Fedrow, C. D. Ott, M. Szczepanczyk, R. Haas, E. Schnetter 1 1 2 3 4 5 2 3 4 5 ~ 240 km ~ 450 km ~ 1200 km ~ 900 km A3O1 A3O3 A3O6 A3O8 YITP/Kyoto U. Caltech ERAU UIUC Perimeter Institute Gravitational Waves from 3D Rotating Core-Collapse Supernovae Credit: P. Mösta et al. 2014, ApJ 785, L29 We present gravitational wave (GW) signals from new general-relativistic 3D simulations of rotating core- collapse supernovae. We use a realistic progenitor model, a microphysical equation of state, and neutrino leakage/heating. We explore the dependence of 3D dynamics and GW emission as a function of the precollapse rotation rate. For rapid rotation resulting in proto-neutron stars with millisecond periods, we find the development of a nonaxisymmetric (m={1,2}) rotational instability that dramatically alters supernova dynamics and GW emission. The next galactic core-collapse supernova will be observed in GWs, neutrinos, and photons. All stars rotate and some massive stars may have rapidly spinning cores. Their quadrupole deformation gives off a GW burst at core bounce when the proto-neutron star is formed. The emitted GW signal is detectable throughout the Milky Way [1] and can constrain core spin [2]. Early 3D simulations (e.g., [3]) showed that in addition to the axisymmetric GW emission at bounce, 3D rotational instability can trigger strong nonaxisymmetric deformation of the proto-neturon star. This can have a dramatic impact on the supernova explosion dynamics [4]. The 3D dynamics results in a strong, quasi-circularly polarized GW signal that dramatically enhances the overall GW emission and thus detectability [3,4]. Abstract Simulations Background We are long overdue for a core-collapse supernova within our galaxy. When it happens we need to know what kind of gravitational waveform to expect. As shown by our numerical relativity simulations, given the right observational conditions, current and next generation gravitational wave detectors will be able to observe the GWs from these core-collapse supernovae events. Conclusions: [email protected] Joseph M. Fedrow, Graduate Student Yukawa Institute for Theoretical Physics Advanced Future Studies Kyoto University, Kyoto, Japan Contact Info: This research is supported in part by the International Research Unit of Advanced Future Studies at Kyoto University and by NSF under award CAREER PHY- 1151197. The simulations were carried out on NSF/NCSA Blue Waters (NSF PRAC award no. ACI- 1440083) and on NSF XSEDE under allocation TG- PHY100033. Acknowledgments [1] Gossan et al. 2016, PRD 93, 042002 [2] Abdikamalov al. 2014, PRD 90, 044001 [3] Ott al. 2007, PRL 98, 261101 [4] Takiwaki et al. 2016, MNRAS 461, L112 [5] Hayama et al. 2016, PRL 116, 151102 [6] Ott et al. 2012, PRD 86, 024026, Ott et al. 2013, ApJ 768, 115 [7] Löffler et al. 2012, CQG 29, 115001 [8] Lattimer & Swesty 1991, Nuc. Phys. A 535, 331 [9] Woosley & Heger 2007, Phys. Rep. 442, 269 References We carry out 3+1 general-relativistic rotating core collapse simulations using the Zelmani core collapse simulation package [6] that is based on the open- source Einstein Toolkit [7]. We employ 8 levels of AMR, the LS 220 equation of state [8] and the 12 M ☉ progenitor of [9]. Electron capture during collapse is included with a Y e (ρ) fit. Neutrino transport after bounce is handled by a leakage/heating scheme [6]. We set up constant angular velocity on cylindrical shells using Ω(r) = Ω 0 [1+(r/A) 2 ] -1 with A = 634 km (A3 of [2]). We vary Ω 0 from 1 rad s -1 (model A3O1) to 8 rad s -1 (model A3O8). These Ω 0 result in rotation rates (T/|W|) of the inner core at bounce of ~0.4% to ~14%. They thus allow us to probe slow to very fast rotation and its impact on core-collapse supernova dynamics and GW signature.

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Transcript of Users/Home/repos/gr21posterfedrow/affinityd/7 21 after ...future/wp-content/... · J.M.Fedrow,...

J. M. Fedrow, C. D. Ott, M. Szczepanczyk, R. Haas, E. Schnetter1

1 2 3 4 5

2 3 4 5

~240

~450

~1200k

~900

A3O1 A3O3 A3O6 A3O8

YITP/Kyoto U. Caltech ERAU UIUC Perimeter Institute

Gravitational Waves from3D Rotating Core-Collapse Supernovae

Credit:P. Mösta et al. 2014, ApJ 785, L29

We present gravitational wave (GW) signals from newgeneral-relativistic 3D simulations of rotating core-collapse supernovae. We use a realistic progenitormodel, a microphysical equation of state, and neutrinoleakage/heating. We explore the dependence of 3Ddynamics and GW emission as a function of theprecollapse rotation rate. For rapid rotation resultingin proto-neutron stars with millisecond periods, wefind the development of a nonaxisymmetric (m={1,2})rotational instability that dramatically alters super-nova dynamics and GW emission.

The next galactic core-collapse supernova will beobserved in GWs, neutrinos, and photons. All starsrotate and some massive stars may have rapidlyspinning cores. Their quadrupole deformation givesoff a GW burst at core bounce when the proto-neutronstar is formed. The emitted GW signal is detectablethroughout the Milky Way [1] and can constrain corespin [2]. Early 3D simulations (e.g., [3]) showed that inaddition to the axisymmetric GW emission at bounce,3D rotational instability can trigger strong non-axisymmetric deformation of the proto-neturon star.This can have a dramatic impact on the supernovaexplosion dynamics [4]. The 3D dynamics results in astrong, quasi-circularly polarized GW signal thatdramatically enhances the overall GW emission andthus detectability [3,4].

Abstract

SimulationsBackground

We are long overdue for a core-collapse supernovawithin our galaxy. When it happens we need toknow what kind of gravitational waveform to expect.As shown by our numerical relativity simulations,given the right observational conditions, current andnext generation gravitational wave detectors will beable to observe the GWs from these core-collapsesupernovae events.

Conclusions:

[email protected]

Joseph M. Fedrow, Graduate StudentYukawa Institute for Theoretical Physics

Advanced Future StudiesKyoto University, Kyoto, Japan

Contact Info:This research is supported in part by the InternationalResearch Unit of Advanced Future Studies at KyotoUniversity and by NSF under award CAREER PHY-1151197. The simulations were carried out onNSF/NCSA Blue Waters (NSF PRAC award no. ACI-1440083) and on NSF XSEDE under allocation TG-PHY100033.

Acknowledgments

[1] Gossan et al. 2016, PRD 93, 042002[2] Abdikamalov al. 2014, PRD 90, 044001[3] Ott al. 2007, PRL 98, 261101[4] Takiwaki et al. 2016, MNRAS 461, L112[5] Hayama et al. 2016, PRL 116, 151102[6] Ott et al. 2012, PRD 86, 024026, Ott et al. 2013, ApJ 768, 115[7] Löffler et al. 2012, CQG 29, 115001[8] Lattimer & Swesty 1991, Nuc. Phys. A 535, 331[9] Woosley & Heger 2007, Phys. Rep. 442, 269

References

We carry out 3+1 general-relativistic rotating corecollapse simulations using the Zelmani core collapsesimulation package [6] that is based on the open-source Einstein Toolkit [7]. We employ 8 levels ofAMR, the LS 220 equation of state [8] and the 12 M☉progenitor of [9]. Electron capture during collapse isincluded with a Ye(ρ) fit. Neutrino transport afterbounce is handled by a leakage/heating scheme [6].We set up constant angular velocity on cylindrical

shells using Ω(r) = Ω0[1+(r/A)2]-1 with A = 634 km(A3 of [2]). We vary Ω0 from 1 rad s-1 (model A3O1) to8 rad s-1 (model A3O8). These Ω0 result in rotationrates (T/|W|) of the inner core at bounce of ~0.4% to~14%. They thus allow us to probe slow to very fastrotation and its impact on core-collapse supernovadynamics and GW signature.