White dwarf structure in $f(R,T,L_m)$ gravity: beyond the Chandrasekhar mass limit
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arXiv
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| Format: | Preprint |
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2025
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| _version_ | 1866910039773544448 |
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| author | Otoniel, Edson Pretel, Juan M. Z. Mota, Clésio E. Flores, César O. V. Alves, Victor B. T. da Silva, Franciele M. |
| author_facet | Otoniel, Edson Pretel, Juan M. Z. Mota, Clésio E. Flores, César O. V. Alves, Victor B. T. da Silva, Franciele M. |
| contents | In this work, we investigate the relativistic structure of white dwarfs (WDs) within the framework of modified gravity theory $f(R, T, L_m) = R + αT L_m$, which introduces a non-minimal coupling between matter and curvature. Using a realistic equation of state (EoS) that includes contributions from a relativistic degenerate electron gas and ionic lattice effects, we solve the modified Tolman-Oppenheimer-Volkoff (TOV) equations for two standard choices of the matter Lagrangian density: $L_m = p$ and $L_m = -ρ$. We show that the extra $αTL_m$ term significantly alters the mass-radius relation of WDs, especially at high central densities $( ρ_c \gtrsim 10^8 - 10^9\,\rm g/cm^3)$, allowing for stable super-Chandrasekhar configurations. In particular, depending on the sign and magnitude of the parameter $α$, the maximum mass can increase or decrease, and in some regimes, the usual critical point indicating the transition from stability to instability disappears. Our findings suggest that $f(R,T,L_m)$ gravity provides a viable framework to explain the existence of massive WDs beyond the classical Chandrasekhar limit. Using Bayesian inference with WD observational data, we further constrain the coupling parameter $α$ for the two choices of the Lagrangian density $L_m$. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2507_18745 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | White dwarf structure in $f(R,T,L_m)$ gravity: beyond the Chandrasekhar mass limit Otoniel, Edson Pretel, Juan M. Z. Mota, Clésio E. Flores, César O. V. Alves, Victor B. T. da Silva, Franciele M. General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena Solar and Stellar Astrophysics In this work, we investigate the relativistic structure of white dwarfs (WDs) within the framework of modified gravity theory $f(R, T, L_m) = R + αT L_m$, which introduces a non-minimal coupling between matter and curvature. Using a realistic equation of state (EoS) that includes contributions from a relativistic degenerate electron gas and ionic lattice effects, we solve the modified Tolman-Oppenheimer-Volkoff (TOV) equations for two standard choices of the matter Lagrangian density: $L_m = p$ and $L_m = -ρ$. We show that the extra $αTL_m$ term significantly alters the mass-radius relation of WDs, especially at high central densities $( ρ_c \gtrsim 10^8 - 10^9\,\rm g/cm^3)$, allowing for stable super-Chandrasekhar configurations. In particular, depending on the sign and magnitude of the parameter $α$, the maximum mass can increase or decrease, and in some regimes, the usual critical point indicating the transition from stability to instability disappears. Our findings suggest that $f(R,T,L_m)$ gravity provides a viable framework to explain the existence of massive WDs beyond the classical Chandrasekhar limit. Using Bayesian inference with WD observational data, we further constrain the coupling parameter $α$ for the two choices of the Lagrangian density $L_m$. |
| title | White dwarf structure in $f(R,T,L_m)$ gravity: beyond the Chandrasekhar mass limit |
| topic | General Relativity and Quantum Cosmology High Energy Astrophysical Phenomena Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2507.18745 |