SGR J1550−5418 BURSTS DETECTED WITH THE FERMI GAMMA-RAY BURST MONITOR DURING ITS MOST PROLIFIC ACTIVITY
SGR J1550−5418 BURSTS DETECTED WITH THE FERMI GAMMA-RAY BURST MONITOR DURING ITS MOST PROLIFIC ACTIVITY
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DOI：
10.1088/0004-637x/749/2/122
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发表时间：
2012-02
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通讯作者：
A. J. Horst;A. J. Horst;C. Kouveliotou;N. Gorgone;Y. Kaneko;M. Baring;S. Guiriec;S. Guiriec;E. Göğüş;J. Granot;J. Granot;J. Granot;A. L. Watts;Lin Lin-Lin;Lin Lin-Lin;Lin Lin-Lin;P. N. Bhat;E. Bissaldi;V. Chaplin;M. Finger;N. Gehrels;M. Gibby;M. Giles;A. Goldstein;D. Gruber;A. Harding;L. Kaper;A. Kienlin;M. Klis;S. McBreen;J. Mcenery;C. Meegan;W. Paciesas;A. Pe’er;R. Preece;E. Ramirez-Ruiz;A. Rau;Stefanie Wachter;C. Wilson-Hodge;P. Woods;R. Wijers
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作者：
A. J. Horst;A. J. Horst;C. Kouveliotou;N. Gorgone;Y. Kaneko;M. Baring;S. Guiriec;S. Guiriec;E. Göğüş;J. Granot;J. Granot;J. Granot;A. L. Watts;Lin Lin-Lin;Lin Lin-Lin;Lin Lin-Lin;P. N. Bhat;E. Bissaldi;V. Chaplin;M. Finger;N. Gehrels;M. Gibby;M. Giles;A. Goldstein;D. Gruber;A. Harding;L. Kaper;A. Kienlin;M. Klis;S. McBreen;J. Mcenery;C. Meegan;W. Paciesas;A. Pe’er;R. Preece;E. Ramirez-Ruiz;A. Rau;Stefanie Wachter;C. Wilson-Hodge;P. Woods;R. Wijers
我们对2009年1月用费米伽马射线爆发监测器探测到的286个SGR J1550−5418爆发进行了详细的时间和时间积分频谱分析，得到了SGR J1550−5418爆发的时间和频谱特性的最大均匀样本。我们利用GBM提供的宽带和高时间分辨率数据相结合的方法对震源性质进行了统计研究。我们确定了所有突发的持续时间、发射时间、占空比和上升时间，并发现它们是典型的SGR突发。我们在光谱分析中探索了不同的模型，得出结论：在8-200keV波段，SGRJ1550−5418爆发的光谱同样可以用光学薄热韧致辐射(OTTB)、具有指数截止的幂定律(康普顿化模型)和两个黑体(BB)函数(BB+BB)来描述。在光谱符合康普顿化模型的情况下，我们得到了−的平均光致发光指数为0.92，接近−的OTTB指数。我们发现康普顿化的E峰与爆发通量和平均通量之间存在反相关。对于BB+BB函数，我们发现两个BB函数的通量和发射面积是相关的。低温BB的发射面积与中子星表面积相当，与温度无关，而高温BB的发射面积要小得多，且发射面积与温度呈反相关。我们将这些爆发的性质与在极端激活期间从其他SGR源观测到的爆发进行了比较，并讨论了我们的结果在磁暴模型中的意义。
We have performed detailed temporal and time-integrated spectral analysis of 286 bursts from SGR J1550−5418 detected with the Fermi Gamma-ray Burst Monitor (GBM) in 2009 January, resulting in the largest uniform sample of temporal and spectral properties of SGR J1550−5418 bursts. We have used the combination of broadband and high time-resolution data provided with GBM to perform statistical studies for the source properties. We determine the durations, emission times, duty cycles, and rise times for all bursts, and find that they are typical of SGR bursts. We explore various models in our spectral analysis, and conclude that the spectra of SGR J1550−5418 bursts in the 8–200 keV band are equally well described by optically thin thermal bremsstrahlung (OTTB), a power law (PL) with an exponential cutoff (Comptonized model), and two blackbody (BB) functions (BB+BB). In the spectral fits with the Comptonized model, we find a mean PL index of −0.92, close to the OTTB index of −1. We show that there is an anti-correlation between the Comptonized Epeak and the burst fluence and average flux. For the BB+BB fits, we find that the fluences and emission areas of the two BB functions are correlated. The low-temperature BB has an emission area comparable to the neutron star surface area, independent of the temperature, while the high-temperature BB has a much smaller area and shows an anti-correlation between emission area and temperature. We compare the properties of these bursts with bursts observed from other SGR sources during extreme activations, and discuss the implications of our results in the context of magnetar burst models.