Jets from Young Stars and Their Impact on Star Formation

使用世界上最现代化的射电望远镜进行观测将有助于科学家了解像我们太阳这样的恒星是如何形成的。 恒星的形成是由于星际空间的气体和尘埃螺旋下降到一个中心物体上（就像水沿着浴缸的排水管流动一样）。然而，与此同时，这些婴儿恒星将超音速气体喷流送回太空。 天文学家现在才开始了解这个复杂的过程。 这项计划的主要研究者（PI）将使用先进的计算机模型来展示这一过程实际上是如何工作的，特别关注非常接近中央年轻星星的区域。他将使用两个大型射电天线阵列的观测结果来测试他的模型，一个在智利，另一个在夏威夷。PI将与研究生一起完成大部分工作。PI和学生还共同致力于在耶鲁大学莱特纳家庭天文台和天文馆为公众扩大项目和展览。图像和视频将被用来教育公众如何从大型射电阵列天文观测帮助我们更好地了解恒星，如我们的太阳，是如何创建的。该提案描述了使用高分辨率的阿尔马和SMA观测原恒星周围的环境（在10-1000 Au尺度）的研究。 目标是解决有关质量组装过程和原恒星反馈对星星形成的影响的关键问题。分子线观测将与辐射传输模型相结合，以确定原恒星周围气体的速度，温度和密度结构如何演变，以及流入和流出过程如何随时间变化。这些模型包括机械反馈，也包括辐射反馈和原恒星附近冲击产生的紫外光子的加热。 这些结果将为我们理解分子云核中星星的形成效率和恒星质量的起源提供信息。 一名研究生将在整个3年的时间内参与这项研究工作。

Observations using some of the world's most modern radio telescopes will be used to help scientists understand how stars like our sun are formed. Stars form as gas and dust from interstellar space spirals down onto a central object (much like water flowing down a bath tub drain). However, at the same time, these baby stars drive supersonic jets of gas back out into space. Astronomers are only now beginning to understand this complex process. The Principal Investigator (PI) on this proposal will use advanced computer models to show how this process actually works, focusing in particular on regions very close to the central young star. He will test his models using observations from two large arrays of radio dishes, one in Chile, the other in Hawaii. The PI will do much of this work with a graduate student. Together, the PI and student also aim to expand programs and exhibitions for the public at Yale's Leitner Family Observatory and Planetarium. Images and videos will be used to educate the public about how astronomical observations from large radio arrays help us better understand how stars, like our Sun, are created.This proposal describes a study of the environment surrounding protostars (on 10-1000 AU scales) using high resolution ALMA and SMA observations. The goal is to address key questions about the mass-assembling process and the impact of protostellar feedback on star formation. Molecular line observations will be combined with radiative transfer models to determine how the velocity, temperature, and density structure of the gas surrounding protostars evolves and how the infall and outflow processes change over time. The models include mechanical feedback but also radiative feedback and heating from ultraviolet photons produced in shocks close to the protostar. The results will inform our understanding of star formation efficiency in molecular cloud cores and the origin of stellar masses. A graduate student will be involved in this research effort throughout its 3-year duration.