Resolving the source of the solar acoustic oscillations: Preparing for the era of the Daniel K. Inouye Solar Telescope

与钟声类似，对太阳表面一部分的激发可以导致声波(声波)在太阳内部传播，并产生在太阳表面其他地方可以观察到的振动。太阳科学家可以使用这些声波通过一种名为日震学的过程来探测太阳的内部深处。在丹尼尔·K·井上太阳望远镜(DKIST)等新的地面太阳望远镜(DKIST)能够观测到的非常小的尺度下，人们对这些声波的来源知之甚少。这项提议将通过对这些源进行数值建模，并使用这些模型来预测将通过望远镜观测到的情况，来研究这些源的详细性质。拟议的研究将支持对下一代太阳科学家的培训。PI和共同PI将共同指导两名研究生，每个学生都获得了太阳现象的理论、建模和观测方面的关键经验。这项计划将通过理论建模和利用邓恩太阳望远镜(DST)的观测相结合的方式来研究太阳声学模式(p模式)。尽管通过日震学使用p模来探测太阳内部，但太阳p模激发源的详细性质还不是很清楚。提出者将开发详细的数值模拟，以确定源激励机制并测试其效率。这些模拟将被用来产生合成光谱，这些合成光谱可以进行测试，以确定它们对压力、温度和速度波动的敏感性。最后，使用DST的观测将被用来搜索这些热力学波动在谱线中的预测特征。提案中概述的工作将为优化丹尼尔·K·井上太阳望远镜(DKIST)的高空间和光谱分辨率能力提供必要的重要准备科学。

Similar to the ringing of a bell, excitations on one portion of the surface of the Sun can cause sound (acoustic) waves to travel through the interior of the Sun and generate vibrations that can be observed elsewhere on the solar surface. Solar scientists can use these acoustic waves to probe the deep interior of the Sun through a process called helioseismology. At the very small size scales that new ground-based solar telescopes such as the Daniel K. Inouye Solar Telescope (DKIST) will be able to observe, little is known about the sources of these acoustic waves. This proposal will investigate the detailed properties of these sources by numerically modeling them and using these models to predict what will be seen through telescope observations. The proposed research will support the training of the next generation of solar scientists. The PI and co-PI will jointly mentor two graduate students, with each student gaining critical experience in the theory, modeling and observation of solar phenomena. This proposal will investigate solar acoustic modes (p-modes) through a combination of theoretical modeling and observation with the Dunn Solar Telescope (DST). Despite the use of p-modes to probe the interior of the Sun through helioseismology, the detailed properties of the sources of solar p-mode excitation are not well known. The proposers will develop detailed numerical simulations to determine the source excitation mechanisms and test their efficiencies. These simulations will be used to generate synthetic spectra, which can be tested to determine their sensitivity to pressure, temperature and velocity fluctuations. Finally, observations with the DST will be used to search for the predicted signatures of these thermodynamic fluctuations in the spectral lines. The work outlined in the proposal will provide important preparatory science necessary to optimize the high spatial and spectral resolution capabilities of the Daniel K. Inouye Solar Telescope (DKIST).