THERMAL EVOLUTION OF HYPERON-MIXED NEUTRON STARS

被引：43
作者：
Tsuruta, S. [1 ]
Sadino, J. [1 ]
Kobelski, A. [1 ]
Teter, M. A. [1 ]
Liebmann, A. C. [1 ]
Takatsuka, T. [2 ]
Nomoto, K. [3 ,4 ]
Umeda, H. [4 ]
机构：
[1] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA
[2] Iwate Univ, Fac Humanities & Social Sci, Morioka, Iwate 0208550, Japan
[3] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan
[4] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan
来源：
ASTROPHYSICAL JOURNAL | 2009年 / 691卷 / 01期
关键词：
dense matter; stars: neutron; X-rays: stars; X-RAY; NUCLEON SUPERFLUIDITY; PROPER MOTION; BARYON; PULSAR; RADIO; EMISSION; EQUATION; MODELS; MATTER;
D O I：
10.1088/0004-637X/691/1/621
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
With the impressive amount of data that have poured out from Chandra and XMM/Newton X-ray space missions, as well as the lower energy band observations, we are now in the position where careful comparison of neutron star thermal evolution theories with observations will help us to distinguish among various competing theories. For instance, the latest theoretical and observational developments probably will contradict with the direct Urca cooling of neutron stars without some exotic particles. In this paper, we investigate one of the remaining possible fast cooling scenarios-direct Urca cooling of neutron stars in the hyperon-mixed phase. We conclude that this cooling scenario is a valid process if hyperon superfluidity is not too weak.
引用
收藏
页码：621 / 632
页数：12
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