2015/10/07 by Kuantay Boshkayev, K. A. Boshkayev, J. A. Rueda +7 · 20 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Black dwarf #Chandrasekhar limit #Degenerate energy levels #Effective temperature #Scientific Research and Discoveries #Sky #Stellar, planetary, and galactic studies #Thermodynamic equilibrium #White dwarf #Work (physics) #astro-ph.SR
paper · pdf · open access · doi:10.1142/s2010194516601290
published in International Journal of Modern Physics Conference Series 41, 1660129 (World Scientific) · submitted to IJMPCS, 7 pages, 4 figures
arxiv created 2015/10/07 · openalex publication_date 2016/01/01 · arxiv updated 2016/04/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Recently, it has been shown by S. M. de Carvalho et al. (2014) that the deviations between the degenerate case and observations were already evident for 0.7-0.8 M[Formula: see text] white dwarfs. Such deviations were related to the neglected effects of finite temperatures on the structure of a white dwarf. Therefore, in this work by employing the Chandrasekhar equation of state taking into account the effects of temperature we show how the total pressure of the white dwarf matter depends on the mass density at different temperatures. Afterwards we construct equilibrium configurations of white dwarfs at finite temperatures. We obtain the mass-radius relations of white dwarfs for different temperatures by solving the Tolman-Oppenheimer-Volkoff equation, and compare them with the estimated masses and radii inferred from the Sloan Digital Sky Survey Data Release 4.