The Ps-e relation of double neutron stars

被引：0

作者：

Dewi, J. D. M. ^{[1
]}

Podsladlowski, Ph. ^{[2
]}

Pols, O. R. ^{[3
]}

机构：

[1] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England

[2] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England

[3] Univ Utrecht, Astron Inst, NL-3508 TA Utrecht, Netherlands

来源：

MULTICOLORED LANDSCAPE OF COMPACT OBJECTS AND THEIR EXPLOSIVE ORIGINS | 2007年 / 924卷

关键词：

neutron star; binary system; pulsars;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The seven Galactic double neutron stars (DNS)s exhibit a relation between the pulsar spin period and the orbital eccentricity. We show that this relation can only be produced if the second neutron star received a kick that is substantially smaller (with a velocity dispersion of less than 50 km s(-1)) than the standard kick received by a single radio pulsar. This demonstrates that the kick mechanism depends on the evolutionary history of the NS progenitor and that the orbital parameters of DNSs are completely determined by the evolution in the preceding helium star - neutron star phase.

引用

页码：656 / +

页数：2

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