White Dwarf Pulsars and Very Massive Compact Ultra Magnetized White Dwarfs

被引：3

作者：

Otoniel, Edson ^{[1
]}

Lobato, R. V. ^{[1
]}

Malheiro, M. ^{[1
]}

Franzon, Bruno ^{[2
]}

Schramm, Stefan ^{[2
]}

Weber, Fridolin ^{[3
,4
]}

机构：

[1] ITA, Dept Fis, BR-12228900 Sao Jose Dos Campos, SP, Brazil

[2] FIAS, Ruth Moufang Str 1, D-60438 Frankfurt, Germany

[3] San Diego State Univ SDSU, Dept Phys, 5500 Campanile Dr, San Diego, CA 92182 USA

[4] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA

来源：

PROCEEDINGS OF THE 7TH INTERNATIONAL WORKSHOP ON ASTRONOMY AND RELATIVISTIC ASTROPHYSICS (IWARA 2016) | 2017年 / 45卷

基金：

美国国家科学基金会; 巴西圣保罗研究基金会;

关键词：

Magnetized White Dwarfs; Poloidal Magnetic Field; Pulsars; Magnetars; EMISSION; MODELS; STARS;

D O I：

10.1142/S2010194517600242

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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-circle dot with an equatorial radius R similar to 1596 Km, a central magnetic field of B-c = 1.74 x 10(14) G and B-s = 3.6 x 1013 G at the stellar surface.

引用

页数：9

共 42 条

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