Stability of compact stars in a uniform density background cloud

Ksh. Newton Singh; S. K. Maurya; A. Errehymy; O. Donmez; K. Myrzakulov; T. T. Smitha

doi:10.1140/epjc/s10052-024-13661-1

2023 Impact factor 4.2

Particles and Fields

Open Access

Eur. Phys. J. C (2024) 84: 1295
https://doi.org/10.1140/epjc/s10052-024-13661-1

Regular Article - Theoretical Physics

Stability of compact stars in a uniform density background cloud

Ksh. Newton Singh¹, S. K. Maurya²^,3, A. Errehymy⁴^a, O. Donmez⁵, K. Myrzakulov⁶^b and T. T. Smitha²

¹ Department of Physics, National Defence Academy, Khadakwasla, 411023, Pune, India
² Department of Mathematical and Physical Sciences, College of Arts and Sciences, University of Nizwa, 616, Nizwa, Sultanate of Oman
³ Research Center of Astrophysics and Cosmology, Khazar University, 41 Mehseti Street, AZ1096, Baku, Azerbaijan
⁴ Astrophysics Research Centre, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag X54001, 4000, Durban, South Africa
⁵ College of Engineering and Technology, American University of the Middle East, 54200, Egaila, Kuwait
⁶ Department of General and Theoretical Physics, L.N. Gumilyov Eurasian National University, 010008, Astana, Kazakhstan

^a abdelghani.errehymy@gmail.com
^b krmyrzakulov@gmail.com

Received: 8 September 2024
Accepted: 28 November 2024
Published online: 20 December 2024

Abstract

We are discussing a scenario where a compact star (neutron star, NS) is embedded in a thin, uniform density background cloud (a remnant cloud after a supernova or a cloud generated from the late stages of a star e.g., a planetary nebula or asymptotic red giant phases) and its effect on the stability of the compact star. Due to the thin background cloud, the spacetime geometry is minimally deformed allowing us to employ the technique of minimal geometric decoupling (MGD). Assuming a uniform background cloud density simplifies the problem, and through the MGD method, one can take $Θ_{t}^{t} = Θ > 0$ $\Theta ^t_t = \Theta > 0$ , where $Θ$ $\Theta$ is the density of the cloud. The background cloud interacts with the compact star through a coupling strength $α$ $\alpha$ . By varying $α$ $\alpha$ , one can tune the cloud density to analyze the stability of the embedded compact star. We found that for $α < 3 \times 10^{- 5}$ $\alpha < 3 \times 10^{-5}$ , all the thermodynamic quantities are well-behaved, indicating a stable configuration. Once the coupling parameter exceeds $3 \times 10^{- 5}$ $3 \times 10^{-5}$ , the adiabatic index drops below $Γ_{max}^{'}$ $\Gamma _{\text {max}}'$ , triggering a gravitational collapse. Beyond this limit of $α$ $\alpha$ , the pressure and speed of sound also become non-physical. At the end, we have used the $M - R$ $$M-R$$ curve generated from the solution to determine the radii of a few compact stars, namely PSR J1614-2230, PSR J0952-0607, GW190814, and GW200210. Furthermore, we have discussed the possibility of the secondary component of GW200210 i.e. the less massive compact object with an upper mass of $3.3 M_{⊙}$ $3.3M_\odot$ , which may be a stellar black hole with a Schwarzschild radius $R_{BH} = 9.746$ $R_{\text {BH}} = 9.746$ km. However, if the mass is $2.83 M_{⊙}$ $2.83M_\odot$ as observed, then its predicted minimum radius is 10.74 km, corresponding to $α = 0$ $\alpha = 0$ . This radius is far beyond $R_{BH} = 8.357$ $R_{\text {BH}} = 8.357$ km and therefore is most probably a massive NS in the mass gap.

© The Author(s) 2024

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