Revisiting the mechanical properties of the nucleon

TL;DR

This paper provides a comprehensive analysis of the energy and pressure distributions inside the nucleon, exploring their definitions in different dynamical frameworks and their implications for stability and astrophysical phenomena.

Contribution

It introduces a novel approach to defining mechanical properties of the nucleon when the average momentum is non-zero, linking hadronic physics to astrophysical contexts.

Findings

Defined energy and pressure distributions in both instant and front forms.

Established conditions for hydrostatic equilibrium and stability.

Connected nucleon mechanics to equations of state in extreme astrophysical environments.

Abstract

We discuss in detail the distributions of energy, radial pressure and tangential pressure inside the nucleon. In particular, this discussion is carried on in both the instant form and the front form of dynamics. Moreover we show for the first time how these mechanical concepts can be defined when the average nucleon momentum does not vanish. We express the conditions of hydrostatic equilibrium and stability in terms of these two and three-dimensional energy and pressure distributions. We briefly discuss the phenomenological relevance of our findings with a simple yet realistic model. In the light of this exhaustive mechanical description of the nucleon, we also present several possible connections between hadronic physics and compact stars, like e.g. the study of the equation of state for matter under extreme conditions and stability constraints.