Compact stars in $f(Q) = Q +\xi Q^2$ gravity
General Relativity (GR) is not the only way gravity can be geometrised. Instead of curvature, the Teleparallel Theory attributes gravity to torsion $T$, which is related to the antysimmetric part of connection, and the Symmetric Teleparallel theory no longer preserves metricity, describing gravity t...
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Main Authors | , |
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Format | Journal Article |
Language | English |
Published |
11.07.2024
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Subjects | |
Online Access | Get full text |
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Summary: | General Relativity (GR) is not the only way gravity can be geometrised.
Instead of curvature, the Teleparallel Theory attributes gravity to torsion
$T$, which is related to the antysimmetric part of connection, and the
Symmetric Teleparallel theory no longer preserves metricity, describing gravity
through the non-metricity tensor $Q_{\alpha\mu\nu}\equiv \nabla_\alpha
g_{\mu\nu}.$ These descriptions give form to what is known as geometrical
trinity of gravity. Recently, the extensions of GR have been intensively
investigated in order to solve the theoretical impasses which have arisen. In
this sense, it is also useful to investigate the extensions of alternative
descriptions of gravity, which leads us to the so-called $f(T)$ and $f(Q)$
gravities. In this paper, we consider a family of $f(Q)$ models and obtain
their corresponding Tolman-Oppenheimer-{Volkoff} equations applied to
{polytropic} stars. Using numerical integration, it is possible to solve a
system of differential equations and calculate, among other things, the maximum
mass and mass-radius relation allowed. In addition, we explicitly show the
non-metricity behavior inside and outside the star. |
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DOI: | 10.48550/arxiv.2407.08884 |