BRIGHT "MERGER-NOVA" FROM THE REMNANT OF A NEUTRON STAR BINARY MERGER: A SIGNATURE OF A NEWLY BORN, MASSIVE, MILLISECOND MAGNETAR

被引：211

作者：

Yu, Yun-Wei ^{[1
]}

Zhang, Bing ^{[2
,3
,4
]}

Gao, He ^{[2
]}

机构：

[1] Cent China Normal Univ, Inst Astrophys, Wuhan 430079, Peoples R China

[2] Univ Nevada, Dept Phys & Astron, Las Vegas, NV 89154 USA

[3] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China

[4] Peking Univ, Dept Astron, Beijing 100871, Peoples R China

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2013年 / 776卷 / 02期

基金：

中国国家自然科学基金;

关键词：

gamma-ray burst: general; stars: neutron; supernovae: general; GAMMA-RAY BURSTS; GRAVITATIONAL-WAVE BURSTS; X-RAY; ENERGY INJECTION; LIGHT CURVES; ELECTROMAGNETIC COUNTERPARTS; AFTERGLOW; NUCLEOSYNTHESIS; EMISSION; SWIFT;

D O I：

10.1088/2041-8205/776/2/L40

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A massive millisecond magnetar may survive the merger of a neutron star (NS) binary, which would continuously power the merger ejecta. We develop a generic dynamic model for the merger ejecta with energy injection from the central magnetar. The ejecta emission (the "merger-nova") powered by the magnetar peaks in the UV band and the peak of the light curve, progressively shifts to an earlier epoch with increasing frequency. A magnetar-powered merger-nova could have an optical peak brightness comparable to a supernova, which is a few tens or hundreds times brighter than the radioactive-powered merger-novae (the so-called macro-nova or kilo-nova). On the other hand, such a merger-nova would peak earlier and have a significantly shorter duration than that of a supernova. An early collapse of the magnetar could suppress the brightness of the optical emission and shorten its duration. Such millisecond-magnetar-powered merger-novae may be detected from NS-NS merger events without an observed short gamma-ray burst, and could be a bright electromagnetic counterpart for gravitational wave bursts due to NS-NS mergers. If detected, it suggests that the merger leaves behind a massive NS, which has important implications for the equation-of-state of nuclear matter.

引用

页数：5

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