船帆座弹片B的朱雀光谱
Suzaku Spectroscopy of Vela Shrapnel B
摘要：
本文介绍了利用朱雀卫星上的XIS对船帆座榴霰弹B的X射线观测。这个弹片是船帆座超新星遗迹的主爆炸波冲击波阵面之外突出的几个类似喷出物碎片的特征之一。弹片B的光谱是很好地代表了一个单一的温度薄的热等离子体在非平衡电离状态。O，Ne和Mg的元素丰度被发现是显着高于太阳的值，支持的弹片B起源于超新星喷出物。O、Ne和Mg相对于Fe的丰度在其太阳值以上增强，而Si相对于Fe的丰度在其太阳值。这一丰度模式与D型弹片相似，只是较轻元素的增加不那么显著，这表明B型弹片与星际介质的混合范围更广。ISM的贡献被认为在尾部区域更大，因为那里的某些元素的绝对丰度相对于弹片头部的绝对丰度被耗尽。
英文摘要：
We present the X-ray observation of Vela shrapnel B with the XIS on board the Suzaku satellite. The shrapnel is one of several ejecta fragment-like features protruding beyond the primary blast wave shock front of the Vela supernova remnant. The spectrum of shrapnel B is well-represented by a single-temperature thin-thermal plasma in a non-equilibrium ionization state. The elemental abundances of O, Ne, and Mg are found to be significantly higher than the solar values, supporting that shrapnel B originates from supernova ejecta. The abundances of O, Ne, and Mg relative to Fe are enhanced above their solar values, while that of Si relative to Fe are at their solar values. This abundance pattern is similar to that in shrapnel D, except that the enhancements of the lighter elements are less prominent, suggesting more extensive mixing with the interstellar medium (ISM) in shrapnel B. The contribution of the ISM is considered to be larger at the trailing region, because the absolute abundances of some elements there are depleted relative to those at the shrapnel's head.
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