The evolution of buoyant magnetic structures in the solar interior

太阳物理学中最大的挑战之一是了解太阳磁通量是如何从太阳中漂浮出来的。从内部深处（由太阳能发电机产生）到表面。到目前为止，太阳物理学家一直认为磁通量可以被建模为离散的磁浮力？磁流管中。最近的研究表明，这种理想化可能是无效的。这里提出的工作将扩展这项工作，并通过将太阳磁通量建模为嵌入在漫射背景场中的磁场浓度来重新思考当前的3D模拟。如果成功，这项工作将导致我们对太阳磁场演化和动力学的理解发生根本性的转变，并提供对太阳发电机的深入了解。这项工作的结果将为DKIST观测新兴太阳磁通量提供理论基础，这是新天文台的主要目标之一。这项工作也将构成博士论文的基础。提出的工作将是建立一个新的模型，用于通过磁浮力机制从太阳内部深处到表面的磁通量传输。特别是，团队将理想的离散磁代替？通量管吗?在漫射背景场中设置更多物理浓度的磁场。磁场线在磁场集中和背景场之间交织，导致与离散磁通管所期望的非常不同的动力学。这可能包括磁浓度上升造成的质量损失，这在磁通管的情况下是禁止的。他们还将增加模拟的保真度，包括磁浓度上升区域的湍流。该团队将把之前的2.5D研究扩展到全3D模拟。这将需要使用在先前的国家科学基金会支持下获得的超级计算设施。该奖项反映了美国国家科学基金会的法定使命，并通过使用基金会的知识价值和更广泛的影响审查标准进行评估，被认为值得支持。

One of the great challenges in solar physics is to understand how solar magnetic flux floats from the Sun?s deep interior (where it is generated by the solar dynamo) to the surface. Until now, solar physicists have assumed that magnetic flux could be modeled as discrete magnetically buoyant ?flux tubes.? Recent research has suggested that this idealization might be invalid. The work proposed here will expand that work, and rethink current 3D simulations by modeling solar magnetic flux as concentrations of magnetic field embedded in a diffuse background field. If successful, the work will lead to a fundamental shift in our understanding of the evolution and dynamics of the solar magnetic field, and provide insight into the solar dynamo. The results of this work will provide a theoretical basis for DKIST observations of emerging solar magnetic flux, which is one of the principal goals of the new observatory. This work will also form the basis of a PhD thesis.The proposed work will be to develop a new model for the transport of magnetic flux from deep in the solar interior to the surface through the mechanism of magnetic buoyancy. In particular, the team will replace the idealization of discrete magnetic ?flux tubes? with more physical concentrations of magnetic field set in a diffuse background field. Field lines interweave between the magnetic concentration and the background field, resulting in very different dynamics from what one would expect with discrete flux tubes. This can include mass loss from the rising magnetic concentration, which is prohibited in the flux tube case. They will also increase the fidelity of the simulation by including turbulence in the region through which the magnetic concentration rises. The team will expand prior 2.5D studies into full 3D simulations. This will require the use of supercomputing facilities which were acquired under prior NSF support.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.