Mathematical model for Sagittarius A* and related Tolman–Oppenheimer–Volkoff equations

Bors, Dorota; Stańczy, Robert

doi:10.1002/mma.9165

Cited by 1 publication

(1 citation statement)

References 35 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Besides applying the TOV equation to compact stars, there are many applications in astrophysics; for example, Gupta et al 28 determined the hydrostatic masses of the Galaxy cluster observed using Chandra X-ray data. Inspired by the new findings of star motions under the influence of dark matter, Bors and Stańczy 29 explore the model representing the interaction of relativistic gravitationally attractive diffusive fermionic particles evaporating at high energy clusters of stellar systems 30 .…”

Section: Introductionmentioning

confidence: 99%

Compact stars with non-uniform relativistic polytrope

Nouh,

Foda,

Aboueisha

2024

Sci Rep

View full text Add to dashboard Cite

This paper presents new relativistic composite polytropic models for compact stars by simultaneously solving Einstein field equations with the polytropic state equation to simulate the spherically symmetric, static matter distribution. Using a non-uniform polytropic index, we get the Tolman–Oppenheimer–Volkoff equation for the relativistic composite polytrope (CTOV). To analyze the star's structure, we numerically solve the CTOV equation and compute the Emden and mass functions for various relativistic parameters and polytropic indices appropriate for neutron stars. The calculation results show that, as the relativistic parameter approaches zero, we recover the well-known Lane-Emden equation from the Newtonian theory of polytropic stars; thus, testing the computational code by comparing composite Newtonian models to those in the literature yields good agreement. We compute composite relativistic models for the neutron star candidates Cen X-3, SAXJ1808.4-3658, and PSR J1614-22304. We compare the findings with various existing models in the literature. Based on the accepted models for PSR J1614-22304 and Cen X-3, the star's core radius is predicted to be between 50 and 60% percent of its total radius, while we found that the radius of the core of star SAXJ1808.4-3658 is around 30% of the total radius. Our findings show that the neutron star structure may be approximated by a composite relativistic polytrope, resulting in masses and radii that are quite consistent with observation.

show abstract

Section: Introductionmentioning

confidence: 99%