How to identify a strange star

被引：88

作者：

Madsen, J ^{[1
]}

机构：

[1] Aarhus Univ, Inst Phys & Astron, DK-8000 Aarhus C, Denmark

来源：

PHYSICAL REVIEW LETTERS | 1998年 / 81卷 / 16期

关键词：

D O I：

10.1103/PhysRevLett.81.3311

中图分类号：

O4 [物理学];

学科分类号：

0702 ;

摘要：

Contrary to young neutron stars, young strange stars are not subject to the r-mode instability which slows rapidly rotating, hot neutron stars to rotation periods near 10 ms via gravitational wave emission. Young millisecond pulsars are therefore likely to be strange stars rather than neutron stars, or at least to contain significant quantities of quark matter in the interior. [S0031-9007(98)07387-6].

引用

页码：3311 / 3314

页数：4

共 26 条

[1] STRANGE STARS [J].

ALCOCK, C ;

FARHI, E ;

OLINTO, A .

ASTROPHYSICAL JOURNAL, 1986, 310 (01) :261-272

[2] A new class of unstable modes of rotating relativistic stars [J].

Andersson, N .

ASTROPHYSICAL JOURNAL, 1998, 502 (02) :708-713

[3]

ANDERSSON N, ASTROPH9805225

[4] ROTATIONAL PROPERTIES OF STRANGE STARS [J].

COLPI, M ;

MILLER, JC .

ASTROPHYSICAL JOURNAL, 1992, 388 (02) :513-520

[5] DAMPING TIMES FOR NEUTRON-STAR OSCILLATIONS [J].

CUTLER, C ;

LINDBLOM, L ;

SPLINTER, RJ .

ASTROPHYSICAL JOURNAL, 1990, 363 (02) :603-611

[6] The u+d<->u+s reaction rate and bulk viscosity of strange matter [J].

Dai, ZG ;

Lu, T .

ZEITSCHRIFT FUR PHYSIK A-HADRONS AND NUCLEI, 1996, 355 (04) :415-420

[7] Axial instability of rotating relativistic stars [J].

Friedman, JL ;

Morsink, SM .

ASTROPHYSICAL JOURNAL, 1998, 502 (02) :714-720

[8]

Glendenning N.K., 1997, COMPACT STARS

[9] BULK VISCOSITY OF STRANGE QUARK MATTER [J].

GOYAL, A ;

GUPTA, VK ;

PRAGYA ;

ANAND, JD .

ZEITSCHRIFT FUR PHYSIK A-HADRONS AND NUCLEI, 1994, 349 (01) :93-98

[10]

HAENSEL P, 1986, ASTRON ASTROPHYS, V160, P121

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