Thermal evolution of neutron stars

被引：0
|
作者：
Miralles, JA [1 ]
Pons, JA
Reddy, S
机构：
[1] Univ Valencia, Dept Astron & Astrophys, E-46003 Valencia, Spain
[2] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY USA
来源：
ASTROPHYSICS AND SPACE SCIENCE | 1998年 / 263卷 / 1-4期
关键词：
D O I：
10.1023/A:1002120025332
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present results from simulations of protoneutron star thermal evolution using neutrino opacities that are consistently calculated with the equation of state. When hyperons are allowed to appear in the system, we obtain metastable configurations that after the deleptonization stage become unstable. Concerning the evolution of old neutron stars, we present the results of our investigation on the effect of the Joule heating due to magnetic field dissipation. We conclude that this mechanism can be efficient in maintaining the surface temperature of the star above 3 x 10(4) - 10(5) K during a very long time (greater than or equal to 100 Myr), comparable with the decay time of the magnetic field.
引用
收藏
页码：291 / 294
页数：4
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