CAREER: The Role of Stellar Feedback in Star Formation

研究小组将编写详细的计算机模型，说明恒星是如何从我们银河系的气体中诞生的。所有恒星都诞生于星系中的大型气体云中，这些气体凝聚成恒星和行星。研究人员将为决定新星质量的物理学编写新的计算机模型。她还将研究邻近的年轻恒星如何通过向周围注入能量来影响彼此和它们的出生环境。证据表明，我们的太阳是由成千上万的兄弟姐妹共同形成的，这可能塑造了我们的太阳？S的属性。然而，为什么像我们的太阳这样的恒星会有这么大的质量，仍然存在争议。她的团队将模拟恒星如何与它们的诞生环境相互作用，并测试不同的恒星质量起源理论。研究人员将对这些模型进行综合观测，并将其与对我们银河系恒星形成区域的望远镜观测进行比较。该项目的教育目标是增加STEM的参与度和多样性。研究人员将使用世界广角望远镜(WWT)教育软件向公众传播最新的令人兴奋的天文发现。她将利用WWT为当地几个服务不足的人群创建互动实验室，还将组织研究培训和每年一次的恒星形成研讨会。该提案旨在探索恒星形成中的两个基本问题：恒星如何获得质量？是什么决定了分子云中的恒星形成率？PI将通过执行包括外流、风和辐射反馈在内的形成星团的多物理数值模拟来解决这些问题。三个关键的科学目标是：1)限制核心质量在设定恒星初始质量函数中的重要性，2)评估反馈对湍流和恒星形成效率的影响，3)使用“苹果对苹果”的比较进行桥梁模拟和观测。研究人员将对模型进行合成观测，并直接与观测进行比较，利用目前和计划中的数千小时的大规模探测，以非常精细的分辨率探测稠密气体和原恒星外流。

The investigator's group will write detailed computer-models of how stars are born from gas in our galaxy. All stars are born in large clouds of gas in galaxies, which condense to form stars and planets. The investigator will write new computer models for the physics that determines the mass of new stars. She will also study how neighboring young stars influence each other and their birth environment by injecting energy into their surroundings. Evidence suggests our Sun formed together with thousands of siblings, which may have shaped our Sun?s properties. However, why stars like our Sun have the masses they do remains debated. Her team will model how stars interact with their birth environment and test different theories for the origin of star masses. The investigator will produce synthetic observations of the models and compare these to telescope observations of star-forming regions in our Milky Way galaxy. The educational goal of the project is to increase participation and diversity in STEM. The investigator will use the World Wide Telescope (WWT) educational software to communicate recent exciting astronomy discoveries to the public. She will use WWT to create interactive labs for several local underserved populations, will also organize research training and organize an annual star formation symposia.The proposal aims to explore two fundamental questions in star formation: How do stars obtain their masses? What sets the star formation rate in molecular clouds? The PI will address these questions by performing multi-physics numerical simulations of forming star clusters including outflow, wind and radiation feedback. The three key science objectives are to 1) constrain the importance of core masses in setting the stellar initial mass function, 2) evaluate the influence of feedback on turbulence and star formation efficiency, and 3) bridge simulations and observations using "apples-to-apples" comparisons. The investigator will produce synthetic observations of the models and compare directly to observations, harnessing thousands of hours of current and planned large- scale surveys probing dense gas, proto-stellar outflows with very fine resolution.