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Anisotropic stellar structure and maximum mass in curvature-matter coupled gravity using embedding class one approach.

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Title: Anisotropic stellar structure and maximum mass in curvature-matter coupled gravity using embedding class one approach.
Authors: Maurya, S. K.1,2 (AUTHOR) sunil@unizwa.edu.om, Chaudhary, Sourav1,3 (AUTHOR) saurav222019@cuh.ac.in, Kumar, Jitendra3 (AUTHOR) jitendark@gmail.com
Source: European Physical Journal C -- Particles & Fields. Dec2025, Vol. 85 Issue 12, p1-20. 20p.
Subjects: Stellar structure, Pulsars, Hydrostatic equilibrium, Gravitational wave astronomy, Gravitation
Abstract: Inspired by the class one solution of Bhar et al. (Eur Phys J C 77:596, 2017) containing a hypergeometric function, we construct a new exact solution satisfying the Karmarkar condition in f (R , L m , T) -gravity theory. The solution maintains finite metric potentials, density, and pressures, yielding a nonsingular and well-behaved stellar structure. Equilibrium and stability are verified using the Tolman–Oppenheimer–Volkoff equation, cracking approach, Harrison–Zeldovich condition, and the adiabatic index criterion Ω r > 4 / 3 . Central density and pressure values ( ∼ 10 15 g/cm 3 and ∼ 10 34 dyne/cm 2 ) confirm physical plausibility. Mass-radius analysis for high-mass pulsars including PSR J0740+6620, PSR J1810+1744, PSR J1748−2446ao, PSR J2215+5135, and GW190814 matches NICER and gravitational-wave constraints, establishing the anisotropic compact star model as stable, realistic, and observationally consistent whose radii lie within the range of 10.5 - 11.8 km. [ABSTRACT FROM AUTHOR]
Copyright of European Physical Journal C -- Particles & Fields is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: Anisotropic stellar structure and maximum mass in curvature-matter coupled gravity using embedding class one approach.
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  Data: <searchLink fieldCode="AR" term="%22Maurya%2C+S%2E+K%2E%22">Maurya, S. K.</searchLink><relatesTo>1,2</relatesTo> (AUTHOR)<i> sunil@unizwa.edu.om</i><br /><searchLink fieldCode="AR" term="%22Chaudhary%2C+Sourav%22">Chaudhary, Sourav</searchLink><relatesTo>1,3</relatesTo> (AUTHOR)<i> saurav222019@cuh.ac.in</i><br /><searchLink fieldCode="AR" term="%22Kumar%2C+Jitendra%22">Kumar, Jitendra</searchLink><relatesTo>3</relatesTo> (AUTHOR)<i> jitendark@gmail.com</i>
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  Data: <searchLink fieldCode="JN" term="%22European+Physical+Journal+C+--+Particles+%26+Fields%22">European Physical Journal C -- Particles & Fields</searchLink>. Dec2025, Vol. 85 Issue 12, p1-20. 20p.
– Name: Subject
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  Data: <searchLink fieldCode="DE" term="%22Stellar+structure%22">Stellar structure</searchLink><br /><searchLink fieldCode="DE" term="%22Pulsars%22">Pulsars</searchLink><br /><searchLink fieldCode="DE" term="%22Hydrostatic+equilibrium%22">Hydrostatic equilibrium</searchLink><br /><searchLink fieldCode="DE" term="%22Gravitational+wave+astronomy%22">Gravitational wave astronomy</searchLink><br /><searchLink fieldCode="DE" term="%22Gravitation%22">Gravitation</searchLink>
– Name: Abstract
  Label: Abstract
  Group: Ab
  Data: Inspired by the class one solution of Bhar et al. (Eur Phys J C 77:596, 2017) containing a hypergeometric function, we construct a new exact solution satisfying the Karmarkar condition in f (R , L m , T) -gravity theory. The solution maintains finite metric potentials, density, and pressures, yielding a nonsingular and well-behaved stellar structure. Equilibrium and stability are verified using the Tolman–Oppenheimer–Volkoff equation, cracking approach, Harrison–Zeldovich condition, and the adiabatic index criterion Ω r > 4 / 3 . Central density and pressure values ( ∼ 10 15 g/cm 3 and ∼ 10 34 dyne/cm 2 ) confirm physical plausibility. Mass-radius analysis for high-mass pulsars including PSR J0740+6620, PSR J1810+1744, PSR J1748−2446ao, PSR J2215+5135, and GW190814 matches NICER and gravitational-wave constraints, establishing the anisotropic compact star model as stable, realistic, and observationally consistent whose radii lie within the range of 10.5 - 11.8 km. [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
  Label:
  Group: Ab
  Data: <i>Copyright of European Physical Journal C -- Particles & Fields is the property of Springer Nature and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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        Value: 10.1140/epjc/s10052-025-15202-w
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      – Code: eng
        Text: English
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        Type: general
      – SubjectFull: Pulsars
        Type: general
      – SubjectFull: Hydrostatic equilibrium
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      – SubjectFull: Gravitational wave astronomy
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      – SubjectFull: Gravitation
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              M: 12
              Text: Dec2025
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              Y: 2025
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