Gravitational Waves from Core-Collapse Supernovae

Abdikamalov, Ernazar; Pagliaroli, G.; Radice, David

doi:10.1007/978-981-15-4702-7_21-1

Cited by 18 publications

(12 citation statements)

References 67 publications

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“…Supernovae produce an electromagnetic signal which provides information about the surface of last scattering for photons, as well as a neutrino signal which is sensitive to the temperature of the supernovae neutrinosphere. Core-collapse supernovae with aspherical mass-energy dynamics are also believed to generate gravitational waves, though a signal has not yet been detected [32] and is expected to be beyond the current detection capabilities unless the supernova occurs close by in our galaxy [33]. Neutron star mergers, on the other hand, produce a stronger gravitational wave signal from both the inspiral (measured by LIGO and VIRGO [5,34]) and the (unmeasured, thus far) postmerger phase [35].…”

Section: Introductionmentioning

confidence: 96%

Light scalars in neutron star mergers

Dev,

Fortin,

Harris

et al. 2021

Preprint

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Due to their unique set of multimessenger signals, neutron star mergers have emerged as a novel environment for studies of new physics beyond the Standard Model (SM). As a case study, we consider the simplest extension of the SM scalar sector involving a light CP-even scalar singlet S mixing with the SM Higgs boson. These S particles can be produced abundantly in neutron star mergers via the nucleon bremsstrahlung process. We show that the S particles may either be trapped in or stream freely out of the merger remnant, depending on the S mass, its mixing with the SM Higgs boson, and the temperature and baryon density in the merger. In the free-streaming region, the scalar S will provide an extra channel to cool down the merger remnant, with cooling timescales as small as O(ms). On the other hand, in the trapped region, the Bose gas of S particles could contribute a larger thermal conductivity than the trapped neutrinos in some parts of the parameter space, thus leading to faster thermal equilibration than expected. Therefore, future observations of the early postmerger phase of a neutron star merger could effectively probe a unique range of the S parameter space, largely complementary to the existing and future laboratory and supernova limits. In view of these results, we hope the merger simulation community will be motivated to implement the effects of light CP-even scalars into their simulations in both the free-streaming and trapped regimes.

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Section: Introductionmentioning

confidence: 96%

Light scalars in neutron star mergers

Dev,

Fortin,

Harris

et al. 2021

Preprint

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“…Whilst the central engines and inner regions of CCSNe have yet to be fully understood, there exist several studies of their progenitors and the subsequent evolution and detection [47,48,49,50]. For stars of mass larger than 8M , evolution normally proceeds through several stages of core burning and then to core collapse once nuclear fusion halts when there are no further burning processes to balance the gravitational attraction.…”

Section: Core Collapse Supernovaementioning

confidence: 99%

Modifications to the signal from a gravitational wave event due to a surrounding shell of matter

Naidoo,

Bishop,

van der Walt

2021

Preprint

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In previous work, we established theoretical results concerning the effect of matter shells surrounding a gravitational wave (GW) source, and we now apply these results to astrophysical scenarios. Firstly, it is shown that GW echoes that are claimed to be present in LIGO data of certain events, could not have been caused by a matter shell. However, it is also shown that there are scenarios in which matter shells could make modifications of order a few percent to a GW signal; these scenarios include binary black hole mergers, binary neutron star mergers, and core collapse supernovae.

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“…Whilst the central engines and inner regions of CCSNe have yet to be fully understood, there exist several studies of their progenitors and the subsequent evolution and detection [16,17,18]. For stars of mass larger than 8M , evolution normally proceeds through several stages of core burning and then to core collapse once nuclear fusion halts when there are no further burning processes to balance the gravitational attraction.…”

Section: Gravitational Waves From Core Col-lapse Supernovaementioning

confidence: 99%

Effect of a low density dust shell on the propagation of gravitational waves

2020

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In this paper we show that there are circumstances in which the damping of gravitational waves (GWs) propagating through a viscous fluid can be highly significant; in particular, this applies to Core Collapse Supernovae (CCSNe). In previous work, we used linearized perturbations on a fixed background within the Bondi-Sachs formalism, to determine the effect of a dust shell on GW propagation. Here, we start with the (previously found) velocity field of the matter, and use it to determine the shear tensor of the fluid flow. Then, for a viscous fluid, the energy dissipated is calculated, leading to an equation for GW damping. It is found that the damping effect agrees with previous results when the wavlength λ is much smaller than the radius r i of the matter shell; but if λ r i , then the damping effect is greatly increased.Next, the paper discusses an astrophysical application, CCSNe. There are several different physical processes that generate GWs, and many models have been presented in the literature. The damping effect thus needs to be evaluated with each of the parameters λ, r i and the coefficient of shear viscosity η, having a range of values. It is found that in most cases there will be significant damping, and in some cases that it is almost complete.

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Gravitational Waves from Core-Collapse Supernovae

Cited by 18 publications

References 67 publications

Light scalars in neutron star mergers

Light scalars in neutron star mergers

Modifications to the signal from a gravitational wave event due to a surrounding shell of matter

Effect of a low density dust shell on the propagation of gravitational waves

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