Connecting Multiwavelength Variability of Protoplanetary Disks and Their Dynamic Host Stars

该团队将利用经典T-Tauri星(CTTS)GM-Aur及其尘埃原始行星盘的一套天文台，研究在不同波长进行的广泛观测。这一长达一个月的数据集收集于2019年12月，是CTTS最大的时间协调观测活动。它包括从无线电到X射线的各种波长的观测。它包括SMARTS 1.5米望远镜、拉斯坎伯雷天文台和ALMA上的ChIron梯形光谱仪的地面观测，以及SWIFT、TESS和哈勃太空望远镜的天基观测。这项工作的目的是了解可变的高能辐射场对原行星盘的影响。此外，该团队将维护和扩大LUMA，这是由PI启动的同行指导计划。该团队还将举办一次职业发展研讨会，重点是来自代表性不足群体的天文学家。这项工作要回答的首要问题是，高能辐射场是否(以及在多大程度上)可以影响原行星盘的演化并影响其性质。该小组尤其感兴趣的是，确定这些辐射场是否会导致化学和结构上的变化。该团队将测量质量吸积率，并检查盘中的吸积结构。他们还将测量吸积过程产生的辐射场，以及吸积柱的结构和照亮圆盘的流动。该团队将使用CHIRON光学光谱分析、LCOGT测光、TESS图像和HST数据。该团队还将在GM AUR圆盘中对CO排放线进行建模。他们将从ALMA获得CO排放数据，并使用圆盘模型来推导圆盘化学，使用共入射UV和X射线光度作为系统的约束。这一奖项反映了NSF的法定使命，并通过使用基金会的智力优势和更广泛的影响审查标准进行评估，被认为值得支持。

The team will study a wide set of observations taken at different wavelengths with a suite of observatories of the Classical T Tauri Star (CTTS) GM Aur and its dusty protoplanetary disk. The month-long dataset, collected in December 2019, represents the largest time-coordinated observation campaign of a CTTS. It comprises observations in wavelengths ranging from the radio to the X-ray. It includes ground-based observations from the CHIRON echelle spectrometer on the SMARTS 1.5 m telescope, the Las Cumbres Observatory and ALMA, as well as space-based observations from Swift, TESS and the Hubble Space Telescope. The objective of the work is to understand the influence of variable high-energy radiation fields on the protoplanetary disk. Additionally, the team will maintain and expand LUMA, a peer mentoring program started by the PI. The team will also conduct a career development workshop focused on astronomers from under-represented groups.The overarching question to be answered by this work is whether (and to what degree) high-energy radiation fields can influence the evolution of a protoplanetary disk and impact its properties. In particular, the team is interested in determining whether there are chemical and structural changes due to these radiation fields. The team will measure mass accretion rates and examine accretion structures in the disk. They will also measure the radiation field generated by the accretion process, as well as the structure of the accretion column and the flow illuminating the disk. The team will use CHIRON optical spectrometry, LCOGT photometry, TESS images, and HST data. The team will also model CO emission lines in the GM Aur disk. They will obtain CO emission data from ALMA and use disk models to derive the disk chemistry, using co-incident UV and X-ray luminosities as constraints on the system.This award reflects NSF's statutory mission and has been deemed worthy of support through evaluation using the Foundation's intellectual merit and broader impacts review criteria.