PHASE DRIFTS OF SUB-PULSES DURING THE 2004 GIANT FLARE OF SGR 1806−20 AND SETTLING OF THE MAGNETIC FIELDS
PHASE DRIFTS OF SUB-PULSES DURING THE 2004 GIANT FLARE OF SGR 1806−20 AND SETTLING OF THE MAGNETIC FIELDS
复制标题
DOI：
10.1088/0004-637x/729/1/1
复制
发表时间：
2010-12
期刊：
影响因子：
--
通讯作者：
Y. Xing;Wenfei Yu
中科院分区：
文献类型：
--
作者：
Y. Xing;Wenfei Yu
我们分析了2004年SGR 1806−20大耀斑期间罗西X射线定时探测器的观测结果。我们研究了X射线波形中的子脉冲的相位演化，发现子脉冲的相位随时间变化，然后逐渐稳定，这可能表明发射区域相对于中子星星表面的漂移，或者在磁场变得稳定之前局部发射几何形状的变化。在初始通量尖峰之后约15 s开始测量的相位漂移的特征e折叠时间尺度在37 s和84 s之间的范围内。这导致了中子星星的磁场的特征时间尺度的第一次测量，以解决后，在巨大的耀斑期间的字段重新配置。
We analyzed the observations of SGR 1806−20 performed with the Rossi X-ray Timing Explorer during its 2004 giant flare. We studied the phase evolution of the sub-pulses identified in the X-ray waveform and found that the sub-pulses varied in phase with time and then gradually settled, which might indicate drifts of the emission regions relative to the neutron star surface, or changes in the local emission geometry before the magnetic field became stable. The characteristic e-folding timescale of the phase drifts measured starting about 15 s following the initial flux spike is in the range between 37 s and 84 s. This leads to the first measurements of the characteristic timescale for the magnetic field of the neutron star to settle after a field reconfiguration during the giant flare.