Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism

Gossan, S. E.; Fuller, Jim; Roberts, Luke F.

doi:10.1093/mnras/stz3243

Cited by 20 publications

(22 citation statements)

References 73 publications

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“…In a typical PNS there are two convectively stable regions, one in the inner core and one that composes the outer shell of the PNS that faces the turbulent post-shock region. According to canonical wave theory Handler (2013) (also see Gossan et al (2020) for a direct application in CCSNe), apart from oscillatory p-modes (where pressure acts as restoring force) at high frequency, these stable regions may also house g-modes at lower frequencies (where buoyancy acts as restoring force). These excitations may emit GWs at select eigenmode frequencies when excited.…”

Section: Source Of the Gwsmentioning

confidence: 99%

Equation of State Dependence of Gravitational Waves in Core-Collapse Supernovae

Andersen,

Zha,

Schneider

et al. 2021

Preprint

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Gravitational waves (GWs) provide unobscured insight into the birthplace of neutron stars (NSs) and black holes in core-collapse supernovae (CCSNe). The nuclear equation of state (EOS) describing these dense environments is yet uncertain, and variations in its prescription affect the proto-neutron star (PNS) and the post-bounce dynamics in CCSNe simulations, subsequently impacting the GW emission. We perform axisymmetric simulations of CCSNe with Skyrme-type EOSs to study how the GW signal and PNS convection zone are impacted by two experimentally accessible EOS parameters, (1) the effective mass of nucleons, m , which is crucial in setting the thermal dependence of the EOS, and (2) the isoscalar incompressibility modulus, K sat . While K sat shows little impact, the peak frequency of the GWs has a strong effective mass dependence due to faster contraction of the PNS for higher values of m owing to a decreased thermal pressure. These more compact PNSs also exhibit more neutrino heating which drives earlier explosions and correlates with the GW amplitude via accretion plumes striking the PNS, exciting the oscillations. We investigate the spatial origin of the GWs and show the agreement between a frequency-radial distribution of the GW emission and a perturbation analysis. We do not rule out overshoot from below via PNS convection as another moderately strong excitation mechanism in our simulations. We also study the combined effect of effective mass and rotation. In all our simulations we find evidence for a power gap near ∼1250 Hz, we investigate its origin and report its EOS dependence.

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Section: Source Of the Gwsmentioning

confidence: 99%

Equation of State Dependence of Gravitational Waves in Core-Collapse Supernovae

Andersen,

Zha,

Schneider

et al. 2021

Preprint

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“…Figure 7 shows the characteristic evolution of N and L 2 for a PNS taken from [32]. These calculations are for a model simulated in 1D (assuming spherical symmetry) for which the shock stalls and explosion is not successful.…”

Section: Protoneutron Star Pulsationsmentioning

confidence: 99%

Gravitational Waves from Core-Collapse Supernovae

Abdikamalov,

Pagliaroli,

Radice

2020

Preprint

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We summarize our current understanding of gravitational wave emission from core-collapse supernovae. We review the established results from multidimensional simulations and, wherever possible, provide back-of-the-envelope calculations to highlight the underlying physical principles. The gravitational waves are predominantly emitted by protoneutron star oscillations. In slowly rotating cases, which represent the most common type of the supernovae, the oscillations are excited by multi-dimensional hydrodynamic instabilities, while in rare rapidly rotating cases, the protoneutron star is born with an oblate deformation due to the centrifugal force. The gravitational wave signal may be marginally visible with current detectors for a source within our galaxy, while future third-generation instruments will enable more robust and detailed observations. The rapidly rotating models that develop non-axisymmetric instabilities may be visible up to a megaparsec distance with the third-generation detectors. Finally, we discuss strategies for multi-messenger observations of supernovae.

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“…As another example that deserves more critical analysis, several works have considered the importance of wave driving, damping, and propagation in the post-shock region, generated by motions within the proto-neutron star (Burrows et al 2006;Harada et al 2017;Gossan et al 2020). For a given wave flux into the gain region, the overall wave pressure gradient again enters the Euler equation for the post-shock flow in a manner similar to the turbulent pressure, except with…”

Section: Combining Rotation and Turbulencementioning

confidence: 99%

The antesonic condition for the explosion of core-collapse supernovae – I. Spherically symmetric polytropic models: stability and wind emergence

Raives

Couch

Greco

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Shock revival in core-collapse supernovae (CCSNe) may be due to the neutrino mechanism. While it is known that in a neutrino-powered CCSN, explosion begins when the neutrino luminosity of the proto-neutron star exceeds a critical value, the physics of this condition in time-dependent, multidimensional simulations are not fully understood. Pejcha & Thompson (2012) found that an 'antesonic condition' exists for time-steady spherically symmetric models, potentially giving a physical explanation for the critical curve observed in simulations. In this paper, we extend that analysis to time-dependent, spherically symmetric polytropic models. We verify the critical antesonic condition in our simulations, showing that models exceeding it drive transonic winds whereas models below it exhibit steady accretion. In addition, we find that (1) high spatial resolution is needed for accurate determination of the antesonic ratio and shock radius at the critical curve, and that low resolution simulations systematically underpredict these quantities, making explosion more difficult at lower resolution; (2) there is an important physical connection between the critical mass accretion rate at explosion and the mass loss rate of the post-explosion wind: the two are directly proportional at criticality, implying that, at criticality, the wind kinetic power is tied directly to the accretion power; (3) the value of the post-shock adiabatic index Γ has a large effect on the length and time scales of the post-bounce evolution of the explosion larger values of Γ result in a longer transition from the accretion to wind phases.

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Wave heating from proto-neutron star convection and the core-collapse supernova explosion mechanism

Cited by 20 publications

References 73 publications

Equation of State Dependence of Gravitational Waves in Core-Collapse Supernovae

Equation of State Dependence of Gravitational Waves in Core-Collapse Supernovae

Gravitational Waves from Core-Collapse Supernovae

The antesonic condition for the explosion of core-collapse supernovae – I. Spherically symmetric polytropic models: stability and wind emergence

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