Mentor

Joseph Moscoso, University of North Carolina at Chapel Hill

Gema Villegas, Florida International University

Publication Date

2024

Document Type

Paper

DOI

10.25776/k26g-n936

Pages

1-4 pp.

Abstract

The Tolman-Oppenheimer-Volkoff (TOV) equations provide a theoretical framework for modeling the structure of neutron stars and white dwarfs in hydrostatic equilibrium. Using Python and MATLAB, we simulate the mass-radius relationship, pressure, and density profiles of these compact stars, focusing on how ionized plasma dynamics contribute to their stability. By incorporating particle simulations into the visualization process, we model the internal forces of neutron stars and white dwarfs, demonstrating how computational tools offer unique insights into these celestial objects. The results align well with theoretical predictions and provide a solid foundation for future studies incorporating additional physical effects such as magnetic fields.

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