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Please use this identifier to cite or link to this item: https://hdl.handle.net/2445/201118
Calculation of the equation of state of neutron star matter
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Symmetric nuclear matter, asymmetric nuclear matter and β-stable nuclear matter are discussed and modeled through a Lagrangian density of relativistic mean field (RMF) theory using a σ meson to describe the attractive interaction between nucleons, a ω meson to describe the repulsive interaction and a ρ meson to describe the asymmetry effects with the NL3 parametrization.
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Treballs Finals de Grau de Física, Facultat de Física, Universitat de Barcelona, Curs: 2023, Tutor: Mario Centelles Aixalà
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HERNÁNDEZ TOLEDO, Adrià. Calculation of the equation of state of neutron star matter. [consulted: 6 of June of 2026]. Available at: https://hdl.handle.net/2445/201118