金属污染白矮星G 29-38 X射线辐射的XMM-牛顿探测
XMM-Newton Detection of X-ray Emission from the Metal-Polluted White Dwarf G 29-38
摘要：
最近对受金属污染的白矮星G29-38的钱德拉X射线数据进行的分析显示，X射线发射可归因于行星体的碎片吸积。鉴于这种探测，我们在这里重新审视G29-38的档案XMM-牛顿观测，由于附近存在相对较亮的X射线源，过去只能从中得出上限。在多个能带中对这些数据的分析允许将G29-38位置处的X射线发射与附近源的发射分离。XMM-牛顿和钱德拉观测中源的相似光谱特性及其空间位移，与G29-38在这些观测之间的自行一致，加强了G29 -38发射X射线的起源。两次观测得到的X射线光度在1- $σ$不确定度范围内是一致的，最佳拟合等离子体温度也是如此。虽然计数是小的，有诱人的证据线发射在0.7-0.8千电子伏的能带从光学薄的热等离子体。最有可能产生这种谱线发射的是16 ° C的Fe络合物。
英文摘要：
A recent analysis of Chandra X-ray data of the metal-polluted white dwarf (WD) G29-38 has revealed X-ray emission that can be attributed to the accretion of debris from a planetary body. In the light of this detection we revisit here archival XMM-Newton observations of G29-38 from which only an upper limit was derived in the past due to the presence of a relatively bright nearby X-ray source. An analysis of these data in multiple energy bands allows disentangling the X-ray emission at the location of G29-38 from that of the nearby source. The similar spectral properties of the source in the XMM-Newton and Chandra observations and their spatial shift, consistent with the proper motion of G29-38 between these observations, strengthen the origin of that X-ray emission from G29-38. The X-ray luminosities from both observations are consistent within 1-$σ$ uncertainties, so too are the best-fit plasma temperatures. Although the count number is small, there is tantalizing evidence for line emission in the 0.7-0.8 keV energy band from an optically-thin hot plasma. The most likely candidate for this line emission would be the Fe complex at 16 Å.
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