Idioma:

Hydrostatic equilibrium configurations of neutron stars in a non-minimal geometry-matter coupling theory of gravity

Carvalho, G. A. ; Moraes, P. H. R. S. ; dos Santos, S. I. ; Gonçalves, B. S. ; Malheiro, M.

The European physical journal. C, Particles and fields, 2020-05, Vol.80 (5), p.1-7, Article 483 [Periódico revisado por pares]

Berlin/Heidelberg: Springer Berlin Heidelberg

Texto completo disponível

Citações Citado por

Enviar para

Título:
Hydrostatic equilibrium configurations of neutron stars in a non-minimal geometry-matter coupling theory of gravity
Autor: Carvalho, G. A. ; Moraes, P. H. R. S. ; dos Santos, S. I. ; Gonçalves, B. S. ; Malheiro, M.
Assuntos: Analysis ; Astronomy ; Astrophysics and Cosmology ; Configurations ; Coupling ; Elementary Particles ; Equations of state ; Equilibrium ; Equilibrium equations ; Flux density ; Gravitation ; Gravity ; Hadrons ; Heavy Ions ; Internal waves ; Mathematical analysis ; Measurement Science and Instrumentation ; Neutron stars ; Neutrons ; Nuclear Energy ; Nuclear interactions ; Nuclear Physics ; Physics ; Physics and Astronomy ; Pulsars ; Quantum Field Theories ; Quantum Field Theory ; Regular Article - Theoretical Physics ; Stiffness ; String Theory
É parte de: The European physical journal. C, Particles and fields, 2020-05, Vol.80 (5), p.1-7, Article 483
Descrição: In this work we analyze hydrostatic equilibrium configurations of neutron stars in a non-minimal geometry-matter coupling (GMC) theory of gravity. We begin with the derivation of the hydrostatic equilibrium equations for the f ( R , L ) gravity theory, where R and L are the Ricci scalar and Lagrangian of matter, respectively. We assume f ( R , L ) = R / 2 + [ 1 + σ R ] L , with σ constant. To describe matter inside neutron stars we assume a relativistic polytropic equation of state p = K ρ γ , with ρ being the energy density, K and γ = 5 / 3 being constants. We also consider the more realistic equation of state (EoS) known as SLy4, which is a Skyrme type one based on effective nuclear interaction. We show that in this theory it is possible to reach the mass of massive pulsars, such as PSR J2215 + 5135, for both equations of state. Also, results for mass-radius relation in GMC gravity are strongly dependent on the stiffness of the EoS.
Editor: Berlin/Heidelberg: Springer Berlin Heidelberg
Idioma: Inglês

Voltar para lista de resultados

Realização: Logos de Redes Sociais:

Hydrostatic equilibrium configurations of neutron stars in a non-minimal geometry-matter coupling theory of gravity

Carvalho, G. A. ; Moraes, P. H. R. S. ; dos Santos, S. I. ; Gonçalves, B. S. ; Malheiro, M.

Berlin/Heidelberg: Springer Berlin Heidelberg

Buscando em bases de dados remotas. Favor aguardar.