Mentor

Joseph Moscoso, University of North Carolina at Chapel Hill

Gema Villegas, Florida International University

Publication Date

2024

Document Type

Paper

DOI

10.25776/84zm-zd52

Pages

1-9 pp.

Abstract

This project investigates the modeling of neutron stars and white dwarfs using polytropic equations of state and relativistic corrections. By integrating relativistic effects into the Tolman-Oppenheimer-Volkoff (TOV) equations, we obtain more accurate predictions of neutron star properties, including mass-radius relationships and neutron degeneracy pressure. Non-relativistic models are inadequate under high pressures. Considering nucleon-nucleon interactions suggests that neutron stars can surpass the Tolman-Oppenheimer-Volkoff limit, theoretically reaching masses up to 2.3 π‘€βŠ™. However, empirical data supports a more realistic mass range of 1.5 to 2.3 π‘€βŠ™. The inclusion of neutron star crust modeling refines these predictions, indicating possible masses up to 1.66 π‘€βŠ™. Numerical solutions of the TOV equations, implemented in Python, are essential for accurate modeling, allowing detailed simulations of complex relativistic conditions and reliable comparisons with observational data. This study underscores the importance of incorporating relativistic and nuclear interactions in stellar models to enhance our understanding of compact stellar objects and to address the limits imposed by relativistic physics.

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