Low Temperature Astrophysics, Supermassive Black Holes, Magnetars, Strange Stars, Magnetic Fields in the Universe and in Compact Stars, Dense Quark and Hadron Matter Physics and Astrophysics, Supernovae, Pulsars, Neutron Stars and White DwarfsOpen Access

White Dwarf Pulsars and Very Massive Compact Ultra Magnetized White Dwarfs

Edson Otoniel

Departamento de Física, Instituto Tecnológico de Aeronáutica (ITA), 12228-900 São José dos Campos, SP, Brazil

E-mail Address: otoniel@ita.br

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R. V. Lobato

Departamento de Física, Instituto Tecnológico de Aeronáutica (ITA), 12228-900 São José dos Campos, SP, Brazil

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M. Malheiro

Departamento de Física, Instituto Tecnológico de Aeronáutica (ITA), 12228-900 São José dos Campos, SP, Brazil

E-mail Address: malheiro@ita.br

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Bruno Franzon

Frankfurt Institute for Advanced Studies (FIAS), Ruth-Moufang-Str. 1, D-60438 Frankfurt am Main, Germany

E-mail Address: franzon@fias.uni.frankfurt.de

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Stefan Schramm

Frankfurt Institute for Advanced Studies (FIAS), Ruth-Moufang-Str. 1, D-60438 Frankfurt am Main, Germany

E-mail Address: schramm@fias.uni-frankfurt.de

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, and

Fridolin Weber

Department of Physics, San Diego State University (SDSU), 5500 Campanile Drive, 92182 San Diego, California, USA

Center for Astrophysics and Space Sciences, University of California at San Diego, 92093 La Jolla, California, USA

E-mail Address: fweber@mail.sdsu.edu

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https://doi.org/10.1142/S2010194517600242Cited by:2 (Source: Crossref)

Abstract

In this work, we discuss white dwarf pulsars found recently making also reference of the possibility of some SGRs/AXPs being part of this class of pulsars. We also study the properties of very massive compact ultra magnetized white dwarfs that could be the progenitors candidates of super luminous type Ia supernovae, and also a previous stage of these white dwarf pulsars before the magnetic field decay.The structure of this ultra magnetized white dwarfs is obtained by solving the Einstein-Maxwell equations with a poloidal magnetic field in a fully general relativistic approach. The stellar interior is composed of a regular crystal lattice made of carbon ions immersed in a degenerate relativistic electron gas. We find that magnetized white dwarfs violate the standard Chandrasekhar mass limit significantly. We obtain a maximum white dwarf mass of around $2.12 M_{⊙}$ with an equatorial radius $R \sim 1596$ Km, a central magnetic field of $B_{c} = 1.74 \times 1 0^{14}$ G and $B_{s} = 3.6 \times 1 0^{13}$ G at the stellar surface.

Keywords:

PACS: 97.20.Rp, 97.60.Gb, 04.40.Dg, 98.70.Qy, 04.25.D−, 97.10.Nf

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Published: 15 August 2017

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This is an Open Access article published by World Scientific Publishing Company. It is distributed under the terms of the Creative Commons Attribution 4.0 (CC-BY) License. Further distribution of this work is permitted, provided the original work is properly cited.

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White Dwarf Pulsars and Very Massive Compact Ultra Magnetized White Dwarfs

Abstract

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