X射线辐照原行星盘的原子诊断
Atomic Diagnostics of X-ray Irradiated Protoplanetary Disks
摘要：
我们研究原子线诊断的内部区域的原行星盘与我们的模型的X射线照射盘的气氛，这是以前用来预测可观察到的水平的NeII和NeIII精细结构的转变在12.81和15.55妈妈。我们将X射线电离理论推广到硫，计算了S、S+、S ~（2+）和硫分子中硫的含量。对于D 'Alessio的普通金牛座T星盘，我们发现，SI的精细结构线在25.55妈妈是低于斯皮策红外光谱仪（IRS）的检测水平，在很大程度上是由于X射线电离的原子S在大气层的顶部，并将其纳入分子接近中平面。我们预测，可观察到的通量的SII 6718/6732 AA禁戒跃迁产生在高层大气中的深度和半径略浅比氖精细结构线。这种和其它禁戒谱线跃迁，如OI 6300/6363 AA和CI 9826/9852 AA谱线，作为X射线辐照磁盘大气的补充诊断。我们还分析了CI，CII和OI的低激发精细结构线的潜在作用，这应该是由SOFIA和Herschel观察。
英文摘要：
We study atomic line diagnostics of the inner regions of protoplanetary disks with our model of X-ray irradiated disk atmospheres which was previously used to predict observable levels of the NeII and NeIII fine-structure transitions at 12.81 and 15.55mum. We extend the X-ray ionization theory to sulfur and calculate the fraction of sulfur in S, S+, S2+ and sulfur molecules. For the D'Alessio generic T Tauri star disk, we find that the SI fine-structure line at 25.55mum is below the detection level of the Spitzer Infrared Spectrometer (IRS), in large part due to X-ray ionization of atomic S at the top of the atmosphere and to its incorporation into molecules close to the mid-plane. We predict that observable fluxes of the SII 6718/6732AA forbidden transitions are produced in the upper atmosphere at somewhat shallower depths and smaller radii than the neon fine-structure lines. This and other forbidden line transitions, such as the OI 6300/6363AA and the CI 9826/9852AA lines, serve as complementary diagnostics of X-ray irradiated disk atmospheres. We have also analyzed the potential role of the low-excitation fine-structure lines of CI, CII, and OI, which should be observable by SOFIA and Herschel.
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