Mean-field dynamo action in protoneutron stars

被引：52

作者：

Bonanno, A

Rezzolla, L

Urpin, V ^{[1
]}

机构：

[1] AF Ioffe Inst Phys & Technol, St Petersburg, Russia

[2] INAF, Osservatorio Astrofis Catania, Catania, Italy

[3] Ist Nazl Fis Nucl, Sez Catania, I-95129 Catania, Italy

[4] SISSA, Int Sch Adv Studies, I-34014 Trieste, Italy

[5] Ist Nazl Fis Nucl, Sez Trieste, Trieste, Italy

[6] Isaac Newton Inst Chile Eastern Europe & Eurasia, St Petersburg, Russia

来源：

ASTRONOMY & ASTROPHYSICS | 2003年 / 410卷 / 03期

关键词：

MHD; pulsars : general; stars : neutron; magnetic fields;

D O I：

10.1051/0004-6361:20031459

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have investigated the turbulent mean-field dynamo action in protoneutron stars that are subject to convective and neutron finger instabilities. While the first one develops mostly in the inner regions of the star, the second one is favoured in the outer regions, where the Rossby number is much smaller and a mean-field dynamo action is more efficient. By solving the mean-field induction equation we have computed the critical spin period below which no dynamo action is possible and found it to be similar to1 s for a wide range of stellar models. Because this critical period is substantially longer than the characteristic spin period of very young pulsars, we expect that a mean-field dynamo will be effective for most protoneutron stars.

引用

页码：L33 / L36

页数：4

共 29 条

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