Influence of pressure anisotropy and non-metricity parameter on mass-radius relation and stability of millisecond pulsar in $f(Q)$ gravity
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arXiv
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| Autori principali: | , , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2024
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| _version_ | 1866916424963850240 |
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| author | Maurya, S. K. Singh, Ksh. Newton Mustafa, G. Govender, M. Errehymy, Abdelghani Aziz, Abdul |
| author_facet | Maurya, S. K. Singh, Ksh. Newton Mustafa, G. Govender, M. Errehymy, Abdelghani Aziz, Abdul |
| contents | In this study we explore the astrophysical implications of pressure anisotropy on the physical characteristics of millisecond pulsars within the framework of $f(Q)$ gravity, {in particular $f(Q)=-α\, Q - β$, where $α$ and $β$ are constants.} Starting off with the field equations for anisotropic matter configurations, we adopt the physically salient Durgapal-Fuloria ansatz together with a well-motivated anisotropic factor for the interior matter distribution. This leads to a nonlinear second order differential equation which is integrated to give the complete gravitational and thermodynamical properties of the stellar object. The resulting model is subjected to rigorous tests to ensure that it qualifies as a physically viable compact object within the $f(Q)$-gravity framework. We study in detail the impact of anisotropy on the mass, radius and stability of the star. Our analyses indicate that our models are well-behaved, singularity-free and can account for the existence of a wide range of observed pulsars with masses ranging from 2.08 to 2.67 $M_{\odot}$, with the upper value being in the so-called {\em mass gap} regime observed in gravitational events such as GW190814. {A comparison of the so-called {\em Symmetric Teleparallel Equivalent to GR} (STEGR) models with classical General Relativity (GR) models reveal that the anisotropy parameter and the sign of $β$ impact on the predicted radii of pulsars. In particular, STEGR models have larger radii than their GR counterparts. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_20011 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Influence of pressure anisotropy and non-metricity parameter on mass-radius relation and stability of millisecond pulsar in $f(Q)$ gravity Maurya, S. K. Singh, Ksh. Newton Mustafa, G. Govender, M. Errehymy, Abdelghani Aziz, Abdul General Relativity and Quantum Cosmology In this study we explore the astrophysical implications of pressure anisotropy on the physical characteristics of millisecond pulsars within the framework of $f(Q)$ gravity, {in particular $f(Q)=-α\, Q - β$, where $α$ and $β$ are constants.} Starting off with the field equations for anisotropic matter configurations, we adopt the physically salient Durgapal-Fuloria ansatz together with a well-motivated anisotropic factor for the interior matter distribution. This leads to a nonlinear second order differential equation which is integrated to give the complete gravitational and thermodynamical properties of the stellar object. The resulting model is subjected to rigorous tests to ensure that it qualifies as a physically viable compact object within the $f(Q)$-gravity framework. We study in detail the impact of anisotropy on the mass, radius and stability of the star. Our analyses indicate that our models are well-behaved, singularity-free and can account for the existence of a wide range of observed pulsars with masses ranging from 2.08 to 2.67 $M_{\odot}$, with the upper value being in the so-called {\em mass gap} regime observed in gravitational events such as GW190814. {A comparison of the so-called {\em Symmetric Teleparallel Equivalent to GR} (STEGR) models with classical General Relativity (GR) models reveal that the anisotropy parameter and the sign of $β$ impact on the predicted radii of pulsars. In particular, STEGR models have larger radii than their GR counterparts. |
| title | Influence of pressure anisotropy and non-metricity parameter on mass-radius relation and stability of millisecond pulsar in $f(Q)$ gravity |
| topic | General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2403.20011 |