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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Exploring physical features of anisotropic strange stars beyond standard maximum mass limit in f (R, T) gravity

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Deb, Debabrata [1] ; Ketov, Sergei V. [2, 3, 4, 5] ; Maurya, S. K. [6] ; Khlopov, Maxim [7, 8, 9, 10] ; Moraes, P. H. R. S. [11] ; Ray, Saibal [12, 13]
Total Authors: 6
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[1] Indian Inst Engn Sci & Technol, Dept Phys, Howrah 711103, W Bengal - India
[2] Tomsk Polytech Univ, Res Sch High Energy Phys, 2a Lenin Ave, Tomsk 634050 - Russia
[3] Tokyo Metropolitan Univ, Dept Phys, Minami Ohsawa 1-1, Hachioji, Tokyo 1920397 - Japan
[4] Vienna Univ Technol, Inst Theoret Phys, Wiedner Hauptstr 8-10-136, A-1040 Vienna - Austria
[5] Univ Tokyo, Kavli Inst Phys & Math Universe IPMU, Chiba 2778568 - Japan
[6] Univ Nizwa, Coll Arts & Sci, Dept Math & Phys Sci, Nizwa 616 - Oman
[7] APC Lab, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13 - France
[8] Southern Fed Univ, Inst Phys, 194 Stachki, Rostov Na Donu 344090 - Russia
[9] Ctr Cosmopartcile Phys Cosm, Kashirskoe Shosse 31, Moscow 115409 - Russia
[10] Natl Res Nucl Univ MEPHI, Moscow State Engn Phys Inst, Kashirskoe Shosse 31, Moscow 115409 - Russia
[11] ITA, Dept Fis, BR-12228900 Sao Jose Dos Campos, SP - Brazil
[12] Govt Coll Engn & Ceram Technol, Dept Phys, Kolkata 700010, W Bengal - India
[13] Maulana Abul Kalam Azad Univ Technol, Dept Nat Sci, Haringhata 741249, W Bengal - India
Total Affiliations: 13
Document type: Journal article
Source: Monthly Notices of the Royal Astronomical Society; v. 485, n. 4, p. 5652-5665, JUN 2019.
Web of Science Citations: 7

We study a specific model of anisotropic strange stars in the modified f (R, T)-type gravity by deriving solutions to the modified Einstein field equations representing a spherically symmetric anisotropic stellar object. We take a standard assumption that f (R, T) = R + 2 chi T, where R is Ricci scalar, T is the trace of the energy-momentum tensor of matter, and. is a coupling constant. To obtain our solution to the modified Einstein equations, we successfully apply the `embedding class one' techniques. We also consider the case when the strange quark matter (SQM) distribution is governed by the simplified MIT bag model equation of state given by p(r) = 1/3 (rho - 4B), where B is bag constant. We calculate the radius of the strange star candidates by directly solving the modified TOV equation with the observed values of the mass and some parametric values of B and chi. The physical acceptability of our solutions is verified by performing several physical tests. Interestingly, besides the SQM, another type of matter distribution originates due to the effect of coupling between the matter and curvature terms in the f (R, T) gravity theory. Our study shows that with decreasing the value of chi, the stellar systems under investigations become gradually massive and larger in size, turning them into less dense compact objects. It also reveals that for chi < 0 the f (R, T) gravity emerges as a suitable theory for explaining the observed massive stellar objects like massive pulsars, super-Chandrasekhar stars, and magnetars, etc., which remain obscure in the standard framework of General Relativity. (AU)

FAPESP's process: 15/08476-0 - Gravitational waves in f(R,T) theories: polarization states and astrophysical sources
Grantee:Pedro Henrique Ribeiro da Silva Moraes
Support type: Scholarships in Brazil - Post-Doctorate