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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

The Structure and Stability of Massive Hot White Dwarfs

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Author(s):
Nunes, Silvia P. [1] ; Arbanil, V, Jose D. ; Malheiro, Manuel [1]
Total Authors: 3
Affiliation:
[1] Ctr Tecn Aerospacial, Inst Tecnol Aeronaut, Dept Fis, BR-12228900 Sao Jose Dos Campos, SP - Brazil
Total Affiliations: 1
Document type: Journal article
Source: ASTROPHYSICAL JOURNAL; v. 921, n. 2 NOV 2021.
Web of Science Citations: 0
Abstract

We investigate the structure and stability against radial oscillations, pycnonuclear reactions, and inverse beta-decay of hot white dwarfs. We consider the fluid matter to be made up of nucleons and electrons confined in a Wigner-Seitz cell surrounded by free photons. It is considered that the temperature depends on the mass density considering the presence of an isothermal core. We find that the temperature produces remarkable effects on the equilibrium and radial stability of white dwarfs. The stable equilibrium configuration results are compared with those for white dwarfs estimated from the Extreme Ultraviolet Explorer survey and the Sloan Digital Sky Survey. We derive masses, radii, and central temperatures for the most massive white dwarfs according to the surface gravity and effective temperature reported by the surveys. We note that these massive stars are in the mass region where general relativity effects are important. These stars are near the threshold of instabilities due to radial oscillations, pycnonuclear reactions, and inverse beta-decay. Regarding the radial stability of these stars as a function of the temperature, we find that it decreases with the increment of central temperature. We also find that the maximum-mass point and the zero eigenfrequencies of the fundamental mode are determined at the same central energy density. Regarding low-temperature stars, pycnonuclear reactions occur in similar central energy densities, and the central energy density threshold for inverse beta-decay is not modified. For T ( c ) >= 1.0 x 10(8) {[}K], the onset of radial instability is attained before pycnonuclear reaction and inverse beta-decay. (AU)

FAPESP's process: 13/26258-4 - Superdense matter in the universe
Grantee:Manuel Máximo Bastos Malheiro de Oliveira
Support Opportunities: Research Projects - Thematic Grants