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

Naidoo, Monos; Bishop, Nigel T.; Walt, Petrus J. van der

doi:10.1007/s10714-021-02841-z

Cited by 5 publications

(5 citation statements)

References 44 publications

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“…As shown in previous work [12,1], solving the vacuum Einstein equations under the condition of no incoming radiation leads to β [2,2] =b 0 , W [2,2]…”

Section: Using Bondi-sachs Formalismsupporting

confidence: 52%

“…We have shown, previously, that a dust shell surrounding a GW event modifies a gravitational (GW) wave in both magnitude and phase [1], and extended the analysis to show that a burst of GWs can, in principle, lead to echoes [2], although, in practice, an astrophysical scenario that would produce a discernible echo is unlikely. We further showed that the results are astrophysically relevant: the GW signal from events including core collapse supernovae (CCSNe) and binary neutron star (BNS) mergers can be changed so that the modification is measurable [2]. A key point about these effects is that the magnitude is proportional to λ/r i , where λ is the GW wavelength and r i is the matter shell radius.…”

Section: Introductionmentioning

confidence: 90%

“…We use the formalism developed previously [1,2] on GWs propagating through matter shells. The metric is in Bondi-Sachs form…”

Section: Using Bondi-sachs Formalismmentioning

confidence: 99%

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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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“…As shown in previous work [12,1], solving the vacuum Einstein equations under the condition of no incoming radiation leads to β [2,2] =b 0 , W [2,2]…”

Section: Using Bondi-sachs Formalismsupporting

confidence: 52%

Section: Introductionmentioning

confidence: 90%

See 1 more Smart Citation

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

2020

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“…We use the formalism developed previously [7,8] on GWs propagating through matter shells. The metric is in Bondi-Sachs form [12,13]…”

Section: Linearized Perturbations In the Bondi-sachs Formalismmentioning

confidence: 99%

“…However, Hawking [3] showed that in the case of nonzero shear viscosity, η, GWs travelling through such a fluid would lose energy to the medium so that the GWs would be damped; see also [4][5][6]. In a series of recent papers, we have shown how a dust shell surrounding a GW event modifies the GWs in both magnitude and phase [7,8]; and that if the matter in the shell is viscous then GWs are damped [9] and the matter heated [10,11]. A key point about these effects is that they can be large and astrophysically significant as λ/r increases, where λ is the GW wavelength and r is the radius of the shell.…”

Section: Introductionmentioning

confidence: 96%

Effect of a viscous fluid shell on the propagation of gravitational waves

2022

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Previous work has shown that the interaction between gravitational waves (GWs) and a shell of viscous matter leads to damping of the GWs and heating of the matter, and that these effects may be astrophysically significant. This result was derived using the theory of linear perturbations about a Minkowki background, and in this work the model is extended to be more physically realistic by allowing the background geometry to be Schwarzschild. It is found that the difference between using a Schwarzschild or Minkowski background is minimal when either r ≫ M or λ < M , where r is the radius of the shell, λ is the GW wavelength and M is the mass of the system in geometric units (so that 1M⊙ = 1.48km). However, when r ∼ 6M and λ ∼ 25M , then the damping and heating effects are about 9 times larger on a Schwarzschild background than on Minkowski, and such situations occur astrophysically.

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Interaction between gravitational waves and a viscous fluid shell on a Schwarzschild background

Bishop

2024

Phys. Rev. D

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

Cited by 5 publications

References 44 publications

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

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

Effect of a viscous fluid shell on the propagation of gravitational waves

Interaction between gravitational waves and a viscous fluid shell on a Schwarzschild background

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