Near-Infrared Spectroscopy of Young Stellar Objects

最年轻的可观测恒星最可靠的特征之一是它们的红外CO光谱线从风或一对准直的双极喷流中发射出来。这种能量流出的来源仍然未知，但有理由相信这种粒子喷射的能量来自于恒星周围吸积盘物质的落入。然后，物质在磁力和恒星旋转力的共同作用下发生偏转，并以准直流的形式喷射出去。本文的目的是研究CO、氢、氧和其他元素的发射谱线，以检验“x加速器”模型的正确性。首席研究员和他的合作研究员刚刚建造了一个高色散红外光谱仪，他们将在夏威夷莫纳克亚天文台的红外望远镜上用于这个项目。他们将使用他们的数据来约束观察到的流动的运动学模型，并与x加速器模型的创始人，加州大学伯克利分校的Frank Shu博士密切合作。这项研究的结果不仅可以应用于年轻的恒星，还可以应用于其他观测到双极喷流的地方，比如“活跃”星系的核心。

One of the most reliable signatures of the youngest observable stars is the emission of their infrared CO spectral lines from a wind or a pair of collimated bipolar jets. The source of this energetic outflow is still unknown, but there are reasons to believe that the energy for this particle ejection comes from the infall of matter from a circumstellar accretion disk. The matter is then deflected by a combination of magnetic and stellar rotation forces and ejected in a collimated flow. The object of this proposal is to study the emission profiles of CO, hydrogen, oxygen, and lines of other elements in order to test the correctness "x-celerator" model. The Principal Investigator and his Co-Investigator have just constructed a high dispersion infrared spectrograph that they will use for this program at the infrared telescopes on Mauna Kea Observatory, Hawaii. They will use their data to constrain the kinematical models for observed flows and work closely with the originator of the x-celerator model, Dr. Frank Shu of U. Calif. Berkeley. The results of this investigation are expected to have application not only to young stars but to other sites where bipolar jets have been observed, such as the nuclei of "active" galaxies.