Magnetized White Dwarfs

Abstract

The purpose of this thesis is to obtain more realistic equations of state to describe the matter forming magnetized white dwarfs, and use them to solve its structure equations. The equations of state are determined by considering the weak magnetic field approximation $B<B_c$ ($B_c=4.41\times 10^{13}\text{ G}$) for the electron gas of the star. The magnetic field introduces anisotropic pressures, even for the moderate values present in white dwarfs. Also, we consider the energy and pressure correction due to the Coulomb interaction of the electron gas with the ions located in a crystal lattice. Moreover, spherically symmetric Tolman-Oppenheimer-Volkoff structure equations are solved independently for the perpendicular and parallel pressures, confirming the necessity of using axisymmetric structure equations, more adequate to describe the anisotropic system. Therefore, we study the solutions in cylindrical coordinates. In this case, the mass per longitude unit is obtained instead of the total mass of the white dwarf.

51 pages, 13 figures, Diploma Thesis in Theoretical Physics, written in Spanish

References in corpus (6)

• Neutron Star Observations: Prognosis for Equation of State Constraints
• Black Holes in Astrophysics
• New mass limit for white dwarfs: super-Chandrasekhar type Ia supernova as a new standard candle
• Maximum mass of stable magnetized highly super-Chandrasekhar white dwarfs: stable solutions with varying magnetic fields
• Static solutions of Einstein's equations with cylindrical symmetry
• The Mass Spectrum of X-Ray Binaries