Hydromagnetic instabilities in proto-neutron stars

被引：39

作者：

Miralles, JA

Pons, JA

Urpin, VA

机构：

[1] Univ Alicante, Dept Fis Aplicada, E-03080 Alicante, Spain

[2] Univ Roma La Sapienza, Dipartimento Fis G Marconi, I-00184 Rome, Italy

[3] Univ Valencia, Dept Astron & Astrofis, E-46100 Burjassot, Spain

[4] AF Ioffe Phys Tech Inst, St Petersburg 194021, Russia

来源：

ASTROPHYSICAL JOURNAL | 2002年 / 574卷 / 01期

关键词：

convection; instabilities; MHD; stars : magnetic fields; stars : neutron;

D O I：

10.1086/340899

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The stability properties of newly born neutron stars, or proto neutron stars (PNSs), are considered. We take into account dissipative processes, such as neutrino transport and viscosity, in the presence of a magnetic field. In order to find the regions of the star subject to different sorts of instability, we derive the general instability criteria and apply them to evolutionary models of PNSs. The influence of the magnetic field on instabilities is analyzed, and the critical magnetic field stabilizing the star is obtained. In light of our results, we estimate the maximum poloidal magnetic field that might be present in young pulsars or magnetars.

引用

页码：356 / 363

页数：8

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