RUI: Dynamic UC HII regions in Sgr B2: Flickering and Ionized Flows

RUI：Sgr B2 中的动态 UC HII 区域：闪烁和电离流

• 批准号: 1211460
• 负责人: Christopher De Pree
• 金额: $ 20.19万
• 依托单位: Agnes Scott College
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2012
• 资助国家: 美国
• 起止时间: 2012-09-01 至 2016-08-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1211460&HistoricalAwards=false
• 关键词: RUI; Dynamic; UC; HII; regions

Dr. De Pree and his team at Agnes Scott College perform observations with the Expanded Very Large Array (EVLA) to study massive star formation. In particular, they investigate radiation flux variations during massive star formation in HII regions (i.e., regions in the interstellar medium in which hydrogen is mainly present as ionized atoms). Massive stars drive processes that enrich the ISM in chemical elements and significantly impact the evolution of galaxies. The Sgr B2 region is one of the most source-rich massive star forming regions in the Milky Way. It contains many morphologically diverse HII regions, and the number of unusual broad line sources make it an ideal laboratory for testing theories of ultra-compact HII region evolution. Recent high-resolution, radiation-hydrodynamic simulations indicate that dense, rotating, accretion flows that are required to form massive stars quickly become gravitationally unstable. This changes the amount of trapped ionizing radiation and the sizes of the associated ultra-compact HII regions. The orbits of dense clumps and filaments near newly born massive stars thus may irregularly trap and expose their ionizing radiation. These objects are optically thick at a wavelength of 2 cm and thus size variations are also expressed as flux changes. Hence over time, a resulting HII region "flickers" in size between being hyper-compact and ultra-compact throughout the main star accretion phase, rather than monotonically expanding. The accretion flow continues for a period ten times longer than the free expansion timescale for an HII region, and the model can address why ultra-compact HII regions do not more rapidly expand and dissipate. It could also explain the observed distribution of morphologies. The Sgr B2 region contains 49 regions that can be imaged at 1.3 cm wavelength, and 25 of these hyper-compact HII regions have physical diameters less than 5000 Astronomical Units. Dr. De Pree and his team will use the EVLA to reimage this large sample of ultra-compact HII regions to: (1) Determine the frequency and magnitude of ultra-compact HII region flux and size fluctuations over about a 20 year time baseline (since 1989) (2) Constrain and test the theoretical models, (3) Observe recombination lines with the improved spectral resolution and bandwidth of the new EVLA correlator, and characterize line profiles and velocity gradients, and (4) Examine the dynamics of sources with especially broad or multiply peaked line profiles. The EVLA has the spatial and the spectral resolution to properly examine the Broad Line Recombination Objects in the crowded Sgr B2 region. Whether or not flickering is detected, these observations will provide the highest resolution, most sensitive radio image of this prototype massive star forming region, and the reduced data will be made publicly available. The EVLA observations will provide a definitive test of the flickering UC HII region model and will be the first attempt to make time-domain (20 year baseline) observations of a large sample of ultra-compact HII regions.Agnes Scott College, with a 30% African American student body is the only women's college in the Southeastern Association for Research in Astronomy (SARA) consortium, and the Physics and Astronomy Department has a record of success in sending women on to graduate work and careers in the sciences. Dr. De Pree and his group are engaged in the well-established outreach program at Bradley Observatory at Agnes Scott College which is connected to area K12 institutions and hosting over 1500 students each year.

德普里博士和他在艾格尼斯斯科特学院的团队利用扩展的甚大阵列(EVLA)进行观测，以研究大质量恒星的形成。特别是，他们研究了HII区(即星际介质中氢主要以电离原子形式存在的区域)中大质量恒星形成期间的辐射通量变化。大质量恒星驱动的过程使ISM中的化学元素丰富，并对星系的演化产生了重大影响。SGR B2区是银河系中来源最丰富的大质量恒星形成区之一。它包含许多形态上不同的HII区，而数量不同寻常的宽线源使其成为检验超紧凑HII区演化理论的理想实验室。最近的高分辨率辐射流体力学模拟表明，形成大质量恒星所需的密集、旋转、吸积流很快就会变得引力不稳定。这改变了俘获的电离辐射的量和相关的超致密HII区域的大小。因此，新生的大质量恒星附近的致密团块和细丝的轨道可能会不规则地捕获和暴露它们的电离辐射。这些物体在波长2厘米处具有光学厚度，因此大小变化也表示为通量变化。因此，随着时间的推移，所产生的HII区域的大小在整个主星吸积阶段的超紧凑和超紧凑之间“闪烁”，而不是单调扩张。吸积流持续的时间比HII区的自由膨胀时间长十倍，该模型可以解释为什么超致密的HII区不能更快地膨胀和消散。这也可以解释观察到的形貌分布。SGR B2区域包含49个可在1.3厘米波长成像的区域，其中25个超紧凑的HII区域的物理直径小于5000个天文单位。De Pree博士和他的团队将利用EVLA对这一大样本的超紧凑HII区重新成像，以：(1)确定超紧凑HII区通量和尺寸波动的频率和幅度，大约20年的时间基线(自1989年以来)；(2)约束和测试理论模型；(3)利用新的EVLA相关器改进的光谱分辨率和带宽观测复合线，并表征线轮廓和速度梯度；以及(4)研究具有特别宽或多峰谱线轮廓的源的动力学。EVLA具有空间和光谱分辨率，可以适当地检查拥挤的SGR B2区域中的宽线重组对象。无论是否检测到闪烁，这些观测都将提供这个大质量恒星形成区原型的最高分辨率、最灵敏的射电图像，并将公开减少的数据。EVLA观测将提供对闪烁的UC HII区域模型的最终测试，并将首次尝试对超紧凑的HII区域进行时间域(20年基线)观测。Agnes Scott学院拥有30%的非裔美国学生，是东南天文学研究协会(SARA)财团中唯一的女子学院，物理和天文学系在成功地将女性送入研究生工作和科学职业生涯方面有着成功的记录。德普里博士和他的团队在艾格尼斯斯科特学院的布拉德利天文台参与了一项久负盛名的外展项目，该项目与K12区的机构相连，每年接待1500多名学生。