The Geometry and Evolution of Low-Mass Star Formation

低质量恒星形成的几何结构和演化

• 批准号: 9909966
• 负责人: Barbara Whitney
• 金额: $ 10万
• 依托单位: SPACE SCIENCE INSTITUTE
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 1999
• 资助国家: 美国
• 起止时间: 1999-07-15 至 2004-06-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9909966&HistoricalAwards=false
• 关键词: Geometry; Evolution; Low; Mass; Star

ABSTRACTAST-9909966Whitney, BarbaraThis project seeks to link theoretical models for low-mass star formation with observational data. Three-dimensional radiation transfer codes will be developed which attempt to take into account that the process of star formation involves extremely non-spherical geometry such as rotationally-modulated collapse to flared disk structures, as well as bi-polar outflows. Several existing theories describing this process will be tested and compared to the newest high-resolution mid-infrared imaging and spectroscopy data that are now available. In previous work, it has been assumed that the spectral energy distribution of a pre-main sequence star indicates a unique evolutionary state. The new computed models will combine imaging, polarization and spectral energy distributions to test this hypothesis, with particular emphasis on identifying the most relevant: (1) infall scenarios; (2) observational signatures of the current paradigm, the magnetic accretion model; (3) dust properties in the circumstellar environment; and (4) binary formation processes.

这个项目试图将低质量星星形成的理论模型与观测数据联系起来。 三维辐射传输代码将试图考虑到星星的形成过程涉及到非常非球形的几何形状，如旋转调制崩溃到喇叭形磁盘结构，以及双极外流。 描述这一过程的几种现有理论将被测试，并与现在可用的最新高分辨率中红外成像和光谱数据进行比较。 在以前的工作中，人们一直假设前主序星星星的光谱能量分布表明了一种独特的演化状态。新的计算模型将结合联合收割机成像、偏振和光谱能量分布来检验这一假设，特别强调确定最相关的：（1）坠落情景;（2）当前范例的观测特征，即磁吸积模型;（3）星周环境中的尘埃特性;（4）双星形成过程。