Study of self-bound compact stars in gravity and observational constraints on the model parameters

S. K. Maurya; Himanshu Chaudhary; Allah Ditta; G. Mustafa; Saibal Ray

doi:10.1140/epjc/s10052-024-12838-y

2024 Impact factor 4.8

Particles and Fields

Open Access

Eur. Phys. J. C (2024) 84: 603
https://doi.org/10.1140/epjc/s10052-024-12838-y

Regular Article - Theoretical Physics

Study of self-bound compact stars in $f (T)$ $f(\mathscr {T})$ gravity and observational constraints on the model parameters

S. K. Maurya¹, Himanshu Chaudhary¹, Allah Ditta², G. Mustafa³^d and Saibal Ray⁴^e

¹ Department of Mathematical and Physical Sciences, College of Arts and Sciences, University of Nizwa, 616, Nizwa, Sultanate of Oman
² Department of Mathematics, Shanghai University and Newtouch Center for Mathematics of Shanghai University, 200444, Shanghai, People’s Republic of China
³ Department of Physics, Zhejiang Normal University, 321004, Jinhua, People’s Republic of China
⁴ Centre for Cosmology, Astrophysics and Space Science (CCASS), GLA University, 281406, Mathura, Uttar Pradesh, India

^d gmustafa3828@gmail.com
^e saibal.ray@gla.ac.in

Received: 4 March 2024
Accepted: 21 April 2024
Published online: 10 June 2024

Abstract

The present study is based on $f (T)$ $f(\mathscr {T})$ gravity, where we impose possible observational constraints on the model parameters to obtain physically plausible features of compact stars, specifically neutron stars. To do so, as a first step, we consider the field equations in the $f (T)$ $f(\mathscr {T})$ gravity framework. We then solve the field equations to generate a set of new exact solutions in $f (T)$ $f(\mathscr {T})$ gravity where model parameters are found by using boundary conditions. A few tests are performed to asses the stability of the model and compare the obtained results with observations of compact stars, in particular with the compact binary merger event GW190814. We observe the maximum mass of the star beyond the $3 M_{⊙}$ $3M_{\odot }$ when the surface density is of the order $10^{14}$ $10^{14}$ gm/cm $^{3}$ $$^3$$ for the higher torsion parameter, which implies that an anisotropic solution in teleparallel gravity is more suitable for modeling of massive compact objects in lower $m a s s - g a p$ $$mass-gap$$ , and thus the model presented herein provides a satisfactory physical scenario with respect to the observational signature.

© The Author(s) 2024

Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/.