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首页> 外文期刊>The Astrophysical journal >EVIDENCE FOR ACCRETION IN THE HIGH-RESOLUTION X-RAY SPECTRUM OF THE T TAURI STAR SYSTEM Hen 3-600
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EVIDENCE FOR ACCRETION IN THE HIGH-RESOLUTION X-RAY SPECTRUM OF THE T TAURI STAR SYSTEM Hen 3-600

机译：T陶里星系统Hen 3-600的高分辨率X射线光谱中有增生的证据

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摘要

We present high-resolution X-ray spectra of the nearby multiple T Tauri star (TTS) system Hen 3-600, obtained with the High Energy Transmission Grating Spectrograph (HETGS) aboard the Chandra X-Ray Observatory. Both principal binary components of Hen 3-600 (A and B, separation 1.4″) were detected in the zeroth-order Chandra HETGS X-ray image. Hen 3-600-A, the component with a large mid-infrared excess, is a factor of ～2-3 fainter in X-rays than Hen 3-600-B, due to a large flare at Hen 3-600-B during our observation. The dispersed X-ray spectra of the two primary components overlap significantly, so spectral analysis was performed primarily on the first-order spectrum of the combined A + B system, with analysis of the individual dispersed spectra limited to regions where the contributions of A and B can be disentangled via cross-dispersion profile fitting. This analysis results in two lines of evidence indicating that the X-ray emission from Hen 3-600 A + B is derived, in part, from accretion processes. (1) The line ratios of He-like O Ⅶ in the spectrum of Hen 3-600 A + B indicate that the characteristic density of its X-ray-emitting plasma is significantly larger than those of coronally active main-sequence and pre-main-sequence stars. (2) A significant component of low-temperature (2-3 MK) plasma is present in the Hen 3-600 A + B spectrum; this "soft excess" appears somewhat stronger in component A. These results for Hen 3-600 A + B are consistent with, although less pronounced than, results obtained from X-ray grating spectros-copy of more rapidly accreting TTS systems. Indeed, all of the emission signatures of Hen 3-600 A + B that are potential diagnostics of accretion activity-from its high-resolution X-ray spectrum, through its UV excess and Hα emission-line strengths, to its weak near-infrared excess-suggest that its components (and component A in particular) represent a transition phase between rapidly accreting, classical T Tauri stars and nonaccreting, weak-lined T Tauri stars.
机译：我们展示了由钱德拉X射线天文台上的高能透射光栅光谱仪（HETGS）获得的附近的多个T陶里星（TTS）系统Hen 3-600的高分辨率X射线光谱。在零阶Chandra HETGS X射线图像中检测到Hen 3-600的两个主要二元组分（A和B，间距1.4英寸）。 Hen 3-600-A是中红外过量较大的成分，在X射线中比Hen 3-600-B暗2-3倍，这是因为Hen 3-600-B的耀斑很大在我们观察期间。两个主要成分的分散X射线光谱显着重叠，因此光谱分析主要是对A + B组合系统的一阶光谱进行的，对单个分散光谱的分析仅限于A和B贡献的区域。 B可以通过交叉分布轮廓拟合解开。该分析产生了两条证据，表明来自Hen 3-600 A + B的X射线发射部分源自吸积过程。 （1）Hen 3-600 A + B光谱中He样O line的线比率表明，其X射线发射等离子体的特征密度显着大于冠状活性主序列和pre-pre主序星。 （2）Hen 3-600 A + B光谱中存在低温（2-3 MK）等离子体的重要组成部分;这种“软过量”在组分A中似乎更强。Hen 3-600 A + B的这些结果与从吸积较快的TTS系统的X射线光栅光谱学获得的结果一致，尽管不那么明显。的确，Hen 3-600 A + B的所有发射特征都可以诊断积碳活动-从其高分辨率X射线光谱，通过其紫外线过量和Hα发射谱线强度到其弱的近红外光谱过度建议其成分（尤其是成分A）代表快速吸积的经典T Tauri星和不吸积的弱衬T Tauri星之间的过渡阶段。

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