Collaborative Research: Intercomparison of 3D MHD simulations of the solar photosphere and observations: a case study in preparation for the DKIST era

合作研究：太阳光球层 3D MHD 模拟与观测的相互比较：为 DKIST 时代做准备的案例研究

• 批准号: 1835958
• 负责人: Viacheslav Sadykov
• 金额: $ 6.05万
• 依托单位: Bay Area Environmental Research Institute
• 依托单位国家: 美国
• 项目类别: Standard Grant
• 财政年份: 2019
• 资助国家: 美国
• 起止时间: 2019-09-01 至 2021-09-30
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=1835958&HistoricalAwards=false
• 关键词: Collaborative; Research; Intercomparison; 3D; MHD

One of the most pressing problems in understanding Earth?s climate is solar irradiance: the amount of light emitted by the Sun. Solar irradiance is the sole source of heating on Earth. If we want to understand our climate, we must understand the source of the sunlight that warms our planet. The proposed work will examine two different high-resolution magnetohydrodynamic models of the Sun in an effort to understand how magnetic variability at small scales (down to tens of kilometers) can affect irradiance. The team will compare the results of the two different models to high-resolution measurements of the Sun from the NSF?s Dunn Solar Telescope and from NASA?s Solar Dynamics Observatory. The result of this work will be a greater understanding of solar irradiance variability, which will lead to a better understanding of the external influences on the Earth?s climate. This work will form the basis of a graduate student?s PhD thesis.The proposed work is to examine the results of two different three-dimensional magnetohydrodynamic simulations of the solar photosphere for solar irradiance at small (~10 km) scales. Simulated spectra will be generated by BAERI?s StellarBox code and from NCAR/HAO?s MURaM code and compared to observations of the Sun from the Dunn Solar Telescope and from the Solar Dynamics Observatory spacecraft. The team will assess the contribution to solar irradiance in certain spectral ranges from magnetic features too small to be resolved in moderate-resolution imaging. They will also examine the effects of different numerical schemes and approximations used in the two different MHD codes to predicted overall irradiance. The overall objective will be to identify the most suitable numerical contributions for advancing irradiance reconstruction and stellar atmosphere models.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.

理解地球最紧迫的问题之一？S气候是太阳辐照度：太阳发出的光量。太阳辐射是地球上唯一的供暖来源。如果我们想要了解我们的气候，我们必须了解使我们的星球变暖的阳光的来源。这项拟议的工作将研究太阳的两个不同的高分辨率磁流体模型，以努力了解小尺度(低至数十公里)的磁可变性如何影响辐射。该团队将把这两个不同模型的结果与美国国家科学基金会S邓恩太阳望远镜和美国宇航局S太阳动力学天文台的高分辨率太阳测量结果进行比较。这项工作的结果将是更好地了解太阳辐照度的变化，这将导致更好地了解外部因素对地球气候的影响？S。这项工作将构成研究生S博士论文的基础。拟议的工作是检验两种不同的太阳光球层三维磁流体动力学模拟在小(~10公里)尺度上的太阳辐射的结果。模拟光谱将由Baeri？S StellarBox程序和NCAR/Hao？S MURaM程序产生，并与邓恩太阳望远镜和太阳动力学天文台航天器的观测结果进行比较。该团队将评估在某些光谱范围内对太阳辐射的贡献，从太小而无法在中等分辨率成像中分辨的磁性特征。他们还将研究在两种不同的MHD代码中使用的不同数值方案和近似对预测总辐照度的影响。总体目标将是确定最合适的数字贡献来推进辐照度重建和恒星大气模型。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。