Abstract
AbstractThis study explores the behavior of compact stars within the framework of $$f(R,L_m,T)$$
f
(
R
,
L
m
,
T
)
gravity, focusing on the functional form $$f(R,L_m,T) = R + \alpha TL_m$$
f
(
R
,
L
m
,
T
)
=
R
+
α
T
L
m
. The modified Tolman–Oppenheimer–Volkoff (TOV) equations are derived and numerically solved for several values of the free parameter $$\alpha $$
α
by considering both quark and hadronic matter—described by realistic equations of state (EoSs). Furthermore, the stellar structure equations are adapted for two different choices of the matter Lagrangian density (namely, $$L_m= p$$
L
m
=
p
and $$L_m= -\rho $$
L
m
=
-
ρ
), laying the groundwork for our numerical analysis. As expected, we recover the traditional TOV equations in General Relativity (GR) when $$\alpha \rightarrow 0$$
α
→
0
. Remarkably, we found that the two choices for $$L_m$$
L
m
have appreciably different effects on the mass-radius diagrams. Results showcase the impact of $$\alpha $$
α
on compact star properties, while final remarks summarize key findings and discuss implications, including compatibility with observational data from NGC 6397’s neutron star. Overall, this research enhances comprehension of $$f(R,L_m,T)$$
f
(
R
,
L
m
,
T
)
gravity’s effects on compact star internal structures, offering insights for future investigations.
Publisher
Springer Science and Business Media LLC
Cited by
1 articles.
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