EMISSION LINES FROM THE GAS DISK AROUND TW HYDRA AND THE ORIGIN OF THE INNER HOLE
EMISSION LINES FROM THE GAS DISK AROUND TW HYDRA AND THE ORIGIN OF THE INNER HOLE
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DOI：
10.1088/0004-637x/735/2/90
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发表时间：
2011-04
期刊：
影响因子：
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通讯作者：
U. Gorti;D. Hollenbach;J. Najita;I. Pascucci
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作者：
U. Gorti;D. Hollenbach;J. Najita;I. Pascucci
我们比较线发射计算的理论磁盘模型与光学亚毫米波长的观测数据的气体盘周围TW Hya和推断的空间分布的质量在气体盘。与观测结果最匹配的模型盘的气体质量范围为10−4至10−5 M（0.06 Au 13.6 eV）。H2纯转动谱线发射主要来自r = 1 ~ 30 Au。[Oi] 63 μm、HCO+和CO纯转动谱线都产生于r = 30-120 Au的外盘。我们讨论了行星形成和光蒸发的原因，在4 Au内的气体和尘埃的表面密度下降。如果存在行星，我们的结果表明行星质量为0.4 -7兆焦，位于0.3 Au。利用我们的光蒸发模型和与观测结果最匹配的表面密度分布，我们估计当前光蒸发的质量损失率为4 × 10 - 9 M/年，剩余的圆盘寿命为1.55亿年。
We compare line emission calculated from theoretical disk models with optical to submillimeter wavelength observational data of the gas disk surrounding TW Hya and infer the spatial distribution of mass in the gas disk. The model disk that best matches observations has a gas mass ranging from ∼10−4 to 10−5 M☉ for 0.06 AU 13.6 eV) flux from TW Hya. H2 pure rotational line emission comes primarily from r ∼ 1 to 30 AU. [O i] 63 μm, HCO+, and CO pure rotational lines all arise from the outer disk at r ∼ 30–120 AU. We discuss planet formation and photoevaporation as causes for the decrease in surface density of gas and dust inside 4 AU. If a planet is present, our results suggest a planet mass ∼4–7 MJ situated at ∼3 AU. Using our photoevaporation models and the best surface density profile match to observations, we estimate a current photoevaporative mass loss rate of 4 × 10−9 M☉ yr−1 and a remaining disk lifetime of ∼5 million years.