Equation of state constraints from neutron stars

被引:5
作者
Lattimer, James M. [1 ]
机构
[1] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA
关键词
neutron stars; equation of state; pulsars;
D O I
10.1007/s10509-007-9381-3
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Recent measurements of thermal radiation from neutron stars have suggested a rather broad range of radiation radii (R infinity = R/ root 1 - 2GM/Rc(2)). Sources in M13 and Omega Cen imply R infinity similar to 12-14 km, but X7 in 47 Tuc implies R infinity similar to 16-20 km and RX J1856-3754 R infinity > 17 km. If these measurements are all correct, only a limited selection of EOS's could be consistent with them, but a broad range of neutron star masses (up to 2 M circle dot) would also be necessary. The surviving equations of state are incompatible with significant softening above nuclear saturation densities, such as would occur with Boson condensates, a low-density quarkhadron transition, or hyperons. Other potential constraints, such as from QPO's, radio pulsar mass and moment of inertia measurements, and neutron star cooling, are compared.
引用
收藏
页码:371 / 379
页数:9
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