SEARCH FOR GRAVITATIONAL WAVE BURSTS FROM SIX MAGNETARS
SEARCH FOR GRAVITATIONAL WAVE BURSTS FROM SIX MAGNETARS
复制标题
DOI：
10.1088/2041-8205/734/2/l35
复制
发表时间：
2011-06-20
影响因子：
7.9
通讯作者：
Yamaoka, K.
中科院分区：
文献类型：
--
作者：
Abadie, J.;Abbott, B. P.;Yamaoka, K.
软伽马中继星（SGR）和异常X射线源星（AXP）被认为是磁星：由极端磁场驱动的中子星。这些罕见的天体的特征是重复的，有时是壮观的伽马射线爆发。爆发机制可能涉及地壳破裂和激发非径向模式，从而发射引力波（GW）。我们提出了一个搜索的结果GW爆发从六个银河系磁星是敏感的中子星星f-模式，被认为是最有效的GW发射振荡模式的紧凑型恒星。其中一个，SGR 0501+4516，可能类似于距离地球1千秒差距，比之前GW搜索中的目标磁星更接近一个数量级。第二个是AXP 1 E 1547.0-5408，其爆发的各向同性能量估计大于10（44）erg，与巨型耀斑相当。我们没有发现任何证据的GW与1279个电磁触发器的样本发生在2006年11月和2009年6月之间的6个磁星，在GW数据从LIGO，处女座，和GEO 600探测器。我们的最低模型相关GW发射能量上限，用于探测器敏感波段中的带限和时限白色噪声爆发，以及f模式振铃（在1090 Hz），分别为3.0 x 10（44）d（1）（2）erg和1.4 x 10（47）d（1）（2）erg，其中d（1）= d（0501）/1 kpc，d（0501）是到SGR 0501+4516的距离。这些对f模GW发射的限制比以前任何时候都要低一个数量级，并且第一次接近SGR巨型耀斑中看到的电磁能量范围。
Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are thought to be magnetars: neutron stars powered by extreme magnetic fields. These rare objects are characterized by repeated and sometimes spectacular gamma-ray bursts. The burst mechanism might involve crustal fractures and excitation of non-radial modes which would emit gravitational waves (GWs). We present the results of a search for GW bursts from six galactic magnetars that is sensitive to neutron star f-modes, thought to be the most efficient GW emitting oscillatory modes in compact stars. One of them, SGR 0501+4516, is likely similar to 1 kpc from Earth, an order of magnitude closer than magnetars targeted in previous GW searches. A second, AXP 1E 1547.0-5408, gave a burst with an estimated isotropic energy >10(44) erg which is comparable to the giant flares. We find no evidence of GWs associated with a sample of 1279 electromagnetic triggers from six magnetars occurring between 2006 November and 2009 June, in GW data from the LIGO, Virgo, and GEO600 detectors. Our lowest model-dependent GW emission energy upper limits for band-and time-limited white noise bursts in the detector sensitive band, and for f-mode ringdowns (at 1090 Hz), are 3.0 x 10(44)d(1)(2) erg and 1.4 x 10(47)d(1)(2) erg, respectively, where d(1) = d(0501)/1 kpc and d(0501) is the distance to SGR 0501+4516. These limits on GW emission from f-modes are an order of magnitude lower than any previous, and approach the range of electromagnetic energies seen in SGR giant flares for the first time.