用CFHT的近红外摄谱仪SPIROU研究原行星盘中气体和年轻恒星吸积/喷射现象的前景
Perspectives for the study of gas in protoplanetary disks and accretion/ejection phenomena in young stars with the near-IR spectrograph SPIROU at the CFHT
摘要：
近红外原子和分子跃迁是追踪年轻恒星周围环境中温暖和炽热气体的有力工具。在原行星盘内部几个天文单位内，以恒星速度迹热气体（T~1500 K）为中心，观测到H_2和H_2O的振转跃迁以及CO的2 μ m泛频跃迁。H2近红外线显示了几公里/秒的探测分子盘风的蓝移。H2线呈现出数百km/s的蓝移，揭示了喷流中的热冲击气体。原子谱线，如10830 A处的HeI谱线和氢的Paschen β和Brakett γ谱线，追踪来自吸积漏斗流和原子盘风的辐射。在近红外线中的明亮禁止原子线，例如[Fe II]，[N I]，[S I]，[S II]和[C I]，追踪喷流中的原子和电离物质。计划用于加拿大-法国-夏威夷望远镜的新的近红外高分辨率摄谱仪SPIROU将提供独特的能力，在一次曝光中将高光谱分辨率（R~75000）与大波长覆盖范围（0.98至2.35微米）结合起来。这将为我们提供同时探测吸积漏斗流、风、喷流和内部盘中的热气体的手段。这就有可能通过监测观察和系统调查的手段及时调查他们的综合行为。SPIROU将是一个强有力的工具，以促进我们对吸积/弹射过程、盘演化和行星形成之间联系的理解。
英文摘要：
Near-IR atomic and molecular transitions are powerful tools to trace the warm and hot gas in the circumstellar environment of young stars. Ro-vibrational transitions of H2 and H2O, and overtone transitions of CO at 2 micron centered at the stellar velocity trace hot (T~1500 K) gas in the inner few AU of protoplanetary disks. H2 near-IR lines displaying a blueshift of a few km/s probe molecular disk winds. H2 lines presenting blueshifts of hundreds of km/s reveal hot shocked gas in jets. Atomic lines such as the HeI line at 10830 A and the Hydrogen Paschen beta and Brakett gamma lines trace emission from accretion funnel flows and atomic disk winds. Bright forbidden atomic lines in the near-IR of species such as [Fe II], [N I], [S I], [S II], and [C I] trace atomic and ionized material in jets. The new near-IR high resolution spectrograph SPIROU planned for the Canada France Hawaii Telescope will offer the unique capability of combining high-spectral resolution (R~75000) with a large wavelength coverage (0.98 to 2.35 micron) in one single exposure. This will provide us with the means of probing accretion funnel flows, winds, jets, and hot gas in the inner disk simultaneously. This opens the exiting possibility of investigating their combined behavior in time by the means of monitoring observations and systematic surveys. SPIROU will be a powerful tool to progress our understanding of the connexion between the accretion/ejection process, disk evolution, and planet formation.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
