由NA I和CO泛频发射线揭示的ESO H $α$ 279 A的内部暖盘
Inner warm disk of ESO H$α$ 279A revealed by NA I and CO overtone emission lines
摘要：
我们目前的近红外，高分辨率光谱分析对平谱YSO（年轻恒星对象）ESO H $α$ 279 a（1.5太阳质量）在巨蛇座恒星形成区，在429 pc的距离。使用浸没光栅红外光谱仪（IGRINS，R=45,000），我们检测到的发射线来自吸积通道流，射流，和内盘。具体来说，我们确定了氢布拉开系复合，[Fe II]，[Fe III]，[Fe IV]，Ca I，Na I，H2，H2O和CO泛音发射线。通过模拟五条CO泛音发射线和Na I发射线的对称双峰谱线，我们发现ESO H $α$ 279 a具有一个活跃吸积的开普勒盘.从我们的开普勒盘模型，我们发现Na I发射线起源于0.04 AU和1.00 AU之间，而CO泛音发射线来自盘的外部，在0.22 AU和3.00 AU之间。结果表明，中性原子Na气体是吸积盘最内层的良好示踪剂。根据Br_γ辐射光度1.78（+-0.31 x10 ^{31} erg/s）的测量结果，我们得到了质量吸积速率为2- 10 × 10 ^{-7} M_solar/yr。
英文摘要：
We present analysis of near-infrared, high-resolution spectroscopy towards the Flat-spectrum YSO (Young Stellar Object) ESO H$α$ 279a (1.5 solar mass) in the Serpens star forming region, at the distance of 429 pc. Using the Immersion GRating INfrared Spectrometer (IGRINS, R=45,000), we detect emission lines originating from the accretion channel flow, jet, and inner disk. Specifically, we identify hydrogen Brackett series recombination, [Fe II], [Fe III], [Fe IV], Ca I, Na I, H2, H2O and CO overtone emission lines. By modeling five bands of CO overtone emission lines, and the symmetric double-peaked line profile for Na I emission lines, we find that ESO H$α$ 279a has an actively accreting Keplerian disk. From our Keplerian disk model, we find that Na I emission lines originate between 0.04 AU and 1.00 AU, while CO overtone emission lines are from the outer part of disk, in the range between 0.22 AU and 3.00 AU. It reveals that the neutral atomic Na gas is a good tracer of the innermost region of the actively accreting disk. We derive a mass accretion rate of 2-10x10^{-7} M_solar/yr from the measured Br_gamma emission luminosity of 1.78(+-0.31)x10^{31} erg/s.
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