The Physics of Flux Emergence on the Sun

太阳表面磁场的起源和出现，以及它与活动区和耀斑的关系，将通过比较理论模型与地面和天基设施收集的数据来研究。该研究有三个主要目标：(1)磁通量如何从太阳内部产生并表现为活跃区域；(2)确定活动区域的哪些物理性质与耀斑最密切相关，以及(3)确定为什么这些物理性质与耀斑相关。先前的研究表明，“扭结不稳定性”与所谓的“d点活跃区”有关，而“d点活跃区”被认为与耀斑活动密切相关。详细的磁流体力学和辐射输运物理将被纳入浮力磁通管的新模型。将这些模型与高分辨率观测结果进行比较，将有力地验证上升的不稳定磁通管与它们的磁根“断开”并显示观测到的d点活动区特性的假设。这项研究的结果很可能适用于其他表现出表面活动的冷恒星。

Fisher, George"The Physics of Flux Emergence on the Sun"AST-9819727The origin and emergence of magnetic fields on the surface of the Sun and its relationship to active regions and flares will be investigated by comparing theoretical models to data collected at ground- and space-based facilities. The study has three main objectives: (1) how magnetic flux emerges from the solar interior and manifests itself as an active region; (2) to determine which physical properties of active regions are most closely associated with flares, and (3) to identify why those physical properties are associated with flares. Previous work has suggested that a 'kink instability' is associated with so-called 'd-spot active regions' thought to be closely associated with flare activity. Detailed magneto-hydrodyamic and radiative transport physics will be incorporated into new models of buoyant magnetic flux tubes. Comparison of these models with high resolution observations will provide a strong test of the hypothesis that rising unstable flux tubes 'disconnect' from their magnetic roots and manifest the observed properties of d-spot active regions. The results of this study are likely to be applicable to other cool stars that exhibit surface activity.