Peculiar lapse of periodic eclipsing event at low-mass X-ray binary GRS 1747-312 during Suzaku observation in 2009
Peculiar lapse of periodic eclipsing event at low-mass X-ray binary GRS 1747-312 during Suzaku observation in 2009
复制标题
2009年朱雀观测期间低质量X射线双星GRS 1747-312周期性食事件的特殊消失
DOI：
10.1093/pasj/psw011
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发表时间：
2016
影响因子：
2.3
通讯作者：
M. Ozaki & Y. Tawara,
中科院分区：
文献类型：
--
作者：
S. Saji;H. Mori;H. Matsumoto;T. Dotani;M. Iwai;Y. Maeda;I. Mitsuishi;M. Ozaki & Y. Tawara,
GRS 1747Kpc 312是球状星系团−-6中的一颗低质量X射线双星，距离地球9.5kpc。在其爆发期间，人们知道会发生周期性的日食。钱德拉和斯威夫特分别于2004年和2013年对喷发进行了观测。XMM-牛顿在2004年观测到了它的静止状态。此外，2009年作为银心测绘观测的一部分，铃鹿观测到GRS 1747−312处于低光度状态，Lx∼为1.2×1035erg，S−1。除xMM-牛顿外，所有观测都包含了所预测的日食时间。我们分析了这些观察的档案数据。在钱德拉和斯威夫特的观测中，我们发现在日食的预期时间，透明的通量减少了。然而，在Suzaku的观测期间，没有明显的迹象表明预测到的日食。在铃鹿观测期间预测的日食的失误可以用非常接近GRS 1747−312的污染源来解释。当GRS 1747−312处于静止状态时，我们观察到来自污染源的X射线，而不是来自GRS 1747−312的X射线。然而，我们没有明确的证据证明我们数据中的污染源。中子星和伴星之间的厚重物质(NH>；1024 cm−2)也可能解释了这一现象，尽管厚重物质的来源尚不清楚。
GRS 1747−312 is a neutron star low-mass X-ray binary in the globular cluster Terzan 6, located at a distance of 9.5 kpc from the Earth. During its outbursts, periodic eclipses were known to occur. Observations for the outbursts were performed with Chandra in 2004 and Swift in 2013. XMM-Newton observed its quiescent state in 2004. In addition, when Suzaku observed it in 2009 as a part of Galactic center mapping observations, GRS 1747−312 was found to be in a low-luminosity state withLx∼ 1.2 × 1035erg s−1. All of the observations except for XMM-Newton included the time of the eclipses predicted. We analyzed archival data of these observations. During the Chandra and Swift observations, we found clear flux decreases at the expected time of the eclipses. During the Suzaku observation, however, there were no clear signs for the predicted eclipses. The lapse of the predicted eclipses during the Suzaku observation can be explained by a contaminant source quite close to GRS 1747−312. When GRS 1747−312 is in the quiescent state, we observe X-rays from the contaminant source rather than from GRS 1747−312. However, we have no clear evidence for the contaminant source in our data. The lapse might also be explained by thick material (NH> 1024cm−2) between the neutron star and the companion star, though the origin of the thick material is not clear.