喷流、吸积、日冕以及所有这些：来自赫比格恒星HD 163296的神秘X射线
Jets, accretion, coronae and all that: The enigmatic X-rays from the Herbig star HD 163296
摘要：
赫比格Ae/Be星（英语：Herbig Ae/Be stars）是一种前主序星，质量在2到8个太阳质量之间。它们的X射线性质是不确定的，而且至今无法解释。我们希望阐明HAeBes的X射线产生机制。我们提出了HAeBe HD 163296的XMM-牛顿观测。我们分析了光变曲线，宽带和光栅光谱，适合排放措施和丰度和应用模型的吸积和风冲击。我们发现三个温度分量范围从0.2 keV到2.7 keV。O VII类He三重态表明在低密度环境中具有弱UV光子场的X射线形成区域，即。e.在恒星表面之上。这使得吸积激波的起源不太可能，相反，我们建议在喷流的底部为软组分和热组分的日冕起源的冲击。每年10^{-10}个太阳质量的物质外流足以为软X射线提供能量。HD 163296被认为是单一的，因此这些数据代表真正的HAeBe X射线发射。HD 163296可能是它的原型。
英文摘要：
Herbig Ae/Be stars (HAeBe) are pre-main sequence objects in the mass range between 2 and 8 solar masses. Their X-ray properties are uncertain and, as yet, unexplained. We want to elucidate the X-ray generating mechanism in HAeBes. We present a XMM-Newton observation of the HAeBe HD 163296. We analyse the light curve, the broad band and the grating spectra, fit emission measures and abundances and apply models for accretion and wind shocks. We find three temperature components ranging from 0.2 keV to 2.7 keV. The O VII He-like triplet indicates a X-ray formation region in a low density environment with a weak UV photon field, i. e. above the stellar surface. This makes an origin in an accretion shock unlikely, instead we suggest a shock at the base of the jet for the soft component and a coronal origin for the hot component. A mass outflow of 10^{-10} solar masses per year is sufficient to power the soft X-rays. HD 163296 is thought to be single, so this data represent genuine HAeBe X-ray emission. HD 163296 might be prototypical for its class.
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