An Undergraduate Approach to the Quantum Hadrodynamics and the Physics of Neutron Stars
arXiv:2508.16789 · doi:10.3390/universe11080276
Abstract
In this tutorial, I discuss how to model a neutron star from the Quantum Hadrodynamics microscopic approach. After a brief discussion about hydrostatic equilibrium, I discuss the role of each meson of the model and how to calculate the corresponding equation of state and the expected values. Each meson is introduced individually. Its effects are analyzed from both an analytical and a numerical point of view. To explicitly show the effects of a given meson, the coupling constant is varied in an arbitrary range before being fixed to reproduce well-known constraints. This work is intended for late undergraduate students as well as early graduate students. The equation of states is obtained from the statistical mechanics formalism, which is more familiar to students at this stage of their research career, instead of the traditional quantum field theory formalism.
open-acess =)
References in corpus (11)
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- Tidal Love numbers of neutron stars
- PSR J0952-0607: The Fastest and Heaviest Known Galactic Neutron Star
- Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
- Relativistic effective interaction for nuclei, giant resonances, and neutron stars
- Neutron star cooling: Theoretical aspects and observational constraints
- Crystallization of the outer crust of a non-accreting neutron star
- A Neutron Star is born
- Role of the symmetry energy slope in neutron stars: exploring the model-dependency
- Decoding rotating neutron stars: Role of the symmetry energy slope