Role of three coupling parameters on maximum mass and stability: Theoretical insights into relativistic massive compact objects in mass gap under f(Q,T) action
Maurya S.K. Errehymy A. Saginayev Y. Myrzakulov K. Ibragimov I. Dauletov A. Rayimbaev J.
September 2025Elsevier B.V.
Physics of the Dark Universe
2025#49
In this study, we embark on an exciting exploration of matter configurations associated with mass gap objects, particularly those emerging from neutron star mergers and the evolution of massive pulsars. Our investigation leverages the framework of f(Q,T) gravity to unravel the intricate physical properties of these enigmatic compact entities, focusing on the phenomenon of gravitational decoupling through both analytical and numerical methodologies. Central to our research is the analysis of coupling parameters ξ1, ξ2, and α – derived from our theoretical model – and their profound impact on the internal matter variables of these compact stars. By scrutinizing these parameters, we uncover critical insights into the structural dynamics and stability of neutron stars, which are significantly dictated by the equations of state governing their matter content. We innovatively approach the θ-sector using the Pseudo-Isothermal dark matter density profile to approximate the ρθ component, drawing inspiration from dark matter halo studies and galaxy rotation curves. Rigorous testing confirms that our resulting model qualifies as a viable compact object within the f(Q,T) gravity framework. Our detailed analyses reveal the compelling influence of the coupling parameters on the mass, radius, and stability of these stars, demonstrating that our models are well-behaved and singularity-free. Notably, they account for a broad spectrum of observed pulsars with masses ranging from 2.08 to 2.67M⊙, with the upper limit situated in the intriguing mass gap regime identified in gravitational events like GW190814. A comparative study of f(Q,T) models against f(Q) models highlights the distinctive roles of the coupling parameters ξ1, ξ2, and α in shaping the predicted radii of pulsars. Specifically, our findings indicate that f(Q,T) models yield smaller radii compared to their f(Q) counterparts, particularly under the influence of ξ1 and α.
Compact star , Exact solution , f(Q, T) gravity , Mass–radius relation
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Department of Mathematical and Physical Sciences, College of Arts and Sciences, University of Nizwa, Nizwa 616, Oman
Astrophysics Research Centre, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Private Bag X54001, Durban, 4000, South Africa
Center for Theoretical Physics, Khazar University, 41 Mehseti Str., AZ, Baku, 1096, Azerbaijan
Department of General and Theoretical Physics, L.N. Gumilyov Eurasian National University, Astana, 010008, Kazakhstan
Kimyo International University in Tashkent, Shota Rustaveli street 156, Tashkent, 100121, Uzbekistan
Alfraganus University, Yukori Karakamish Street 2a, Tashkent, 100190, Uzbekistan
New Uzbekistan University, Movarounnahr Street 1, Tashkent, 100007, Uzbekistan
Urgench State University, Kh. Alimjan Str. 14, Urgench, 221100, Uzbekistan
Department of Mathematical and Physical Sciences
Astrophysics Research Centre
Center for Theoretical Physics
Department of General and Theoretical Physics
Kimyo International University in Tashkent
Alfraganus University
New Uzbekistan University
Urgench State University
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