Search arXiv⌕ Search

arXiv · gr-qc/0307101

Detection of a close supernova gravitational wave burst in a network of interferometers, neutrino and optical detectors

Abstract

Trying to detect the gravitational wave (GW) signal emitted by a type II supernova is a main challenge for the GW community. Indeed, the corresponding waveform is not accurately modeled as the supernova physics is very complex; in addition, all the existing numerical simulations agree on the weakness of the GW emission, thus restraining the number of sources potentially detectable. Consequently, triggering the GW signal with a confidence level high enough to conclude directly to a detection is very difficult, even with the use of a network of interferometric detectors. On the other hand, one can hope to take benefit from the neutrino and optical emissions associated to the supernova explosion, in order to discover and study GW radiation in an event already detected independently. This article aims at presenting some realistic scenarios for the search of the supernova GW bursts, based on the present knowledge of the emitted signals and on the results of network data analysis simulations. Both the direct search and the confirmation of the supernova event are considered. In addition, some physical studies following the discovery of a supernova GW emission are also mentioned: from the absolute neutrino mass to the supernova physics or the black hole signature, the potential spectrum of discoveries is wide.

Explore related subjects

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Nicolas Arnaud, Matteo Barsuglia, Marie-Anne Bizouard, Violette Brisson, Fabien Cavalier, Michel Davier, Patrice Hello, Stephane Kreckelbergh, Edward K. Porter. 2003-12-19. Detection of a close supernova gravitational wave burst in a network of interferometers, neutrino and optical detectors. https://doi.org/10.1016/j.astropartphys.2003.12.005

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Massive quantum divergence on the Cauchy horizon of a black hole

We investigate a quantum {\it massive} scalar field in the interior of a charged and spherically-symmetric (Reissner-Nordström) black hole. We examine the behaviour for varying values of the black hole charge, field mass and coupling constant when the field is in two quantum states: Hartle-Hawking (representing a black hole in thermal equilibrium) and Unruh (representing a black hole evaporating via the emission of Hawking radiation). We show that the vacuum polarization (in both states) generically {\it diverges} on the Cauchy horizon, in stark contrast to what happens for massless fields; also, the angular components of the quantum stress-energy tensor generically {\it diverge} on the Cauchy horizon and, in at least one of the two states, they do so more strongly than for massless fields. Furthermore, we calculate the energy fluxes in Eddington-Finkelstein coordinates $\{u,v\}$. We show that these fluxes in both states on the Cauchy horizon do not generically vanish. This implies, in particular, that in regular, Kruskal coordinates $\{U,V\}$ the ingoing flux diverges like $V^{-2}$ on the Cauchy horizon (where $V=0$). This divergence suggests that its backreaction via the semiclassical Einstein equations would yield a strong singularity, as opposed to its weaker, classical counterpart. Interestingly, there are exceptions, in which the energy fluxes in Eddington-Finkelstein coordinates vanish: (i) in the extremal limit (where the black hole is maximally charged); (ii) certain fine-tuned regions of parameter space, where the fluxes change sign.

gr-qc↗

Scattering of massless scalar waves by higher-dimensional regular black holes in general relativity coupled to nonlinear electrodynamics

We study the scattering of planar massless scalar waves by the family of higher-dimensional regular black holes in general relativity coupled to nonlinear electrodynamics, which unifies the Bardeen and Hayward models in any dimension. The scalar field is a neutral test field that propagates in the bulk, and in the geometric-optics limit, its rays are the null geodesics of the spacetime, so that the unstable circular null geodesics of the background geometry control the scattering. We combine the classical scattering of null geodesics, the glory approximation, which we generalize to $D$ dimensions, and the partial-wave analysis in $D=5,6,7$. We show that at a fixed frequency, the wave cross section diverges in the forward direction as $θ^{-4}$ in any dimension, with a coefficient fixed by the mass, while the steeper classical law $θ^{-(D-2)^{2}/(D-3)}$ appears only at larger angles and higher frequencies. The charge parameter decreases the critical and the glory impact parameters and widens the glory fringes, and in higher dimensions, the glory pattern has fewer and wider fringes and a weaker backward intensity. For the matched configurations studied here, backward intensity and low-frequency absorption provide the clearest differences, while the intermediate-to-high-frequency spectra are close.

gr-qc↗

Self-interacting $p$-forms and the shear-free anisotropic cosmological model

The cosmological principle may require more than observations demand: what is needed is isotropic expansion without vorticity. Extended Friedmann-Lemaitre-Robertson-Walker (eFLRW) cosmologies realise this with a non-vanishing anisotropic spatial curvature that is balanced by an anisotropic stress while the shear vanishes. Thorsrud and others investigated such scenarios for free differential $p$-forms. Here we extend the analysis to non-Abelian $p$-forms ($p=0,\dots,4$) with self interactions. The balance requires the anisotropic stress to decay as $a^{-2}$, $a$ being the cosmological scale factor, which we combine with the gauge-field continuity equation. The general results indicate that, in the presence of a potential, fine-tuning of the same is needed in order to balance the curvature. Notably, this is not the case for a $3$-form field $\underline{H}^a$ with a potential term $V(\underline{H}^2)=A+B\,\underline{H}^2$, where $A$ and $B$ are constants: in Bianchi class A, an uncharged 3-form balances the curvature with this potential without any tuning, and a charged one does so for a suitably chosen connection. This is the only candidate we have found where the potential does not require tuning. It is also an interesting candidate as it can be interpreted as a cosmological constant in combination with a dark-matter sector mimicking curvature.

gr-qc↗