Search arXiv⌕ Search
Home/Archive/arXiv

arXiv · gr-qc/0512064

Can lightning be a noise source for a spherical gravitational wave antenna?

Nadja S. Magalhaes·Rubem M. Marinho Jr.·Odylio D. Aguiar·C. Frajuca
View original source ↗Read source document ↗Export metadata ↓

Abstract

The detection of gravitational waves is a very active research field at the moment. In Brazil the gravitational wave detector is called Mario SCHENBERG. Due to its high sensitivity it is necessary to model mathematically all known noise sources so that digital filters can be developed that maximize the signal-to-noise ratio. One of the noise sources that must be considered are the disturbances caused by electromagnetic pulses due to lightning close to the experiment. Such disturbances may influence the vibrations of the antenna's normal modes and mask possible gravitational wave signals. In this work we model the interaction between lightning and SCHENBERG antenna and calculate the intensity of the noise due to a close lightning stroke in the detected signal. We find that the noise generated does not disturb the experiment significantly.

Explore related subjects

gr-qc

Keep this discovery

Explore connections, maps & timelines

BibTeXRIS

Nadja S. Magalhaes, Rubem M. Marinho Jr., Odylio D. Aguiar, C. Frajuca. 2005-12-11. Can lightning be a noise source for a spherical gravitational wave antenna?. https://doi.org/10.1103/physrevd.72.102003

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

KEEP EXPLORING

Related papers

arXiv2026

Healthy scalar-tensor theories with third-order derivatives: Generalized disformal Horndeski and beyond

We systematically construct a broad class of ghost-free scalar-tensor theories whose Lagrangian includes up to third-order derivatives of the scalar field. Using a spatially covariant action written in terms of the ADM variables, we impose degeneracy and consistency conditions that remove the additional Ostrogradsky degree of freedom and leave one scalar and two tensor degrees of freedom within the regular branch considered in this paper. The resulting class extends the generalized disformal Horndeski and U-DHOST families.

gr-qc↗
arXiv2026

A class of $d$-dimensional regular black holes: Shadows, Thermodynamics and Gravitational collapse

We investigate a general class of $d$-dimensional regular black holes characterized by a de Sitter core, which arises from the gravitational collapse of a polytropic star with an arbitrary polytropic index $n$. This framework generalizes the well-known Bardeen and Hayward black holes to higher dimensions and identifies nonlinear electrodynamics with a magnetic monopole charge as the physical source ensuring curvature regularity. Geometric structure and energy conditions, demonstrate that while the Weak and Null Conditions are satisfied, the Strong Energy Condition is violated, a necessary feature for curvature singularity avoidance. Our study of optical properties reveals the existence of stable and unstable photon spheres, with shadows persisting only up to a critical magnetic charge limit; beyond this threshold, the object becomes a horizonless compact object. Numerical results indicate that the shadow size decreases as the dimension $d$, charge $q$, or index $n$ increases, allowing for constraints based on EHT observations of M87* and SgrA*. Thermodynamically, unlike the unstable Schwarzschild-Tangherlini solution, these regular black holes exhibit regions of local stability and phase transitions, with entropy deviating from the standard area law in higher dimensions. Finally, we generalize the Oppenheimer-Snyder-Datt collapse scenario to this background. We track the evolution of horizons, and derive a critical lower bound for the initial stellar radius required for physical black hole formation. Our results show that increasing dimensions and the polytropic index delay the collapse proper time, while magnetic charge facilitates the process by reducing the minimum initial radius. These findings provide new insights into the viability of curvature-regular black holes as possible curvature-singularity-free endpoints of gravitational collapse in higher-dimensional gravity.

gr-qc↗
arXiv2026

When Black Holes Can Wear Pants

We investigate the conditions under which black hole fragmentation, the splitting of a black hole horizon into multiple smaller ones, may occur. The simplest realization is that of a single black hole horizon splitting into two, giving rise to the eponymous pants topology. In classical general relativity, the Bekenstein-Hawking area law forbids such processes for Schwarzschild black holes. For spinning Kerr black holes, purely kinematic analyses impose constraints that prevent fragmentation, even in regimes where entropy considerations might allow it, except possibly in near-extremal cases. We then hunt for scenarios where black holes can wear pants: from the well-known Gregory-Laflamme instability in higher dimensions, to the potential effect of superradiant instabilities in non-axisymmetric radiation trapping, to finally gravitational models that modify the relations between entropy and/or horizon radius and the black hole mass in four dimensions. In all such cases, emission of small fragments can be entropically favored, however its occurrence still depends on the kinematic configuration of the initial state. Our analysis clarifies the theoretical landscape where black holes may fragment, which is particularly relevant for primordial black holes and catastrophic events such as black hole mergers.

gr-qc↗