2014/10/31 by Débora P. Menezes, A. Deppman, Airton Deppman +2 · 1 citation
Earth and Planetary Sciences · Mathematics · Physics and Astronomy · #Astrophysics #Baryon #Dense matter #Effective temperature #Equation of state #High-pressure geophysics and materials #Mathematics #Neutron star #Physics #Pulsars and Gravitational Waves Research #Star (game theory) #Stars #Statistical Mechanics and Entropy #Statistical physics #Statistics #Stellar evolution #Strangeness #Thermodynamics #Value (mathematics) #Work (physics) #astro-ph.SR #hep-ph #nucl-th
paper · pdf · doi:10.1140/epja/i2015-15155-3
published as Eur. Phys. J. A 51 (2015) 155 · 13 pages, 9 figures, 3 tables
arxiv created 2015/11/30 · openalex publication_date 2015/12/01 · arxiv updated 2015/12/02 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
In the present work we apply non-extensive statistics to obtain equations of state suitable to describe stellar matter and verify its effects on microscopic and macroscopic quantities. Two snapshots of the star evolution are considered and the direct Urca process is investigated with two different parameter sets. q-values are chosen as 1.05 and 1.14. The equations of state are only slightly modified, but the effects are enough to produce stars with slightly higher maximum masses. The onsets of the constituents are more strongly affected and the internal stellar temperature decreases with the increase of the q-value, with consequences on the strangeness and cooling rates of the stars.