ARE NEUTRON-STARS Q-STARS

被引：33

作者：

BAHCALL, S

LYNN, BW

SELIPSKY, SB

机构：

[1] Department of Physics, Stanford University, Stanford

来源：

NUCLEAR PHYSICS B | 1990年 / 331卷 / 01期

关键词：

D O I：

10.1016/0550-3213(90)90018-9

中图分类号：

O412 [相对论、场论]; O572.2 [粒子物理学];

学科分类号：

摘要：

We show that certain classical solutions of hadronic effective field theories can model neutron stars. Within the uncertainties of what is known from laboratory measurements of nuclear physics, these solutions, called Q-stars, may have masses much larger (≫ 3 M ⊙) or may be able to rotate faster (Prot < 0.5 ms) than previously believed possible. Stable chunks of nuclear density baryonic matter varying in size from 10-12 cm to several kilometers may also exist. Cygnus X-1, LMC X-3, and the SN1987A remnant are candidates for Q-stars. © 1990.

引用

页码：67 / 79

页数：13

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