But for the gravitational physicist, the most exciting aspect of a neutron star is its strong gravitational field, second only to that of a black hole. The estimated strength of a neutron star's gravitational field is so large that Einstein's theory of general relativity manifests itself, ...
The parameters a and b are taken of order 1 km 2 . Arguments are given which suggest that the effective theory so obtained might be a fair approximation of a viable theory. A numerical integration is performed of the field equations for a free neutron gas. The result is that the star ...
Neutron Star Mountains Neutron stars, the remnants of collapsed stars, are extraordinarily dense—about a trillion times denser than lead. Despite their significance, little is known about their surface features. Drawing parallels from mountain-building mechanisms observed on moons and planets in our so...
This paper explores the structure of neutron stars within the framework of \( f(Q) \) gravity theory, a modified gravitational theory that generalizes General Relativity by introducing a function \(…
So I think a neutron star configuration is where we really need to go. In essence the theory would not require a central object. As stated only one apparatus is the trick. Compressing the space, nominally in two planes, and leaving the third plane less compressed. This would side-step ...
unstable-equilibrium neutron star configurationComplete tensor-scalar and hydrodynamic equations are presented and integrated, for a self-gravitating perfect fluid. The initial conditions describe unstable-equilibrium neutron star configuration, with a polytropic equation of state. They are necessary in order...
The structure of neutron starEquation of stateUsing the AV18 equation of state, we numerically calculate the structure of a neutron star in Rastall gravity. The results show that the parameter λ originated from Rastall gravity has a great effect on the mass and the radius of a neutron star...
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[65], serve as constraints on the model parameters. Additionally, deviations in the mass-radius relation can be probed through X-ray observations by NICER and future missions [66]. Moreover, gravitational wave signals from binary neutron star mergers, particularly post-merger oscillations, may ...
Keywords: tidal Love number; neutron star; unimodular gravity 1. Introduction The tidal deformability, or equivalently the tidal Love number (TLN), characterizes the degree of the response of a body to an external tidal force [1]. The observations of gravitational waves from the coalescing neutron...