利用表面磁通输运模型成功重现太阳轨道器极区磁场观测
Successfully Reproducing Solar Orbiter Polar Field Observations with a Surface Flux Transport Model
- Beihang University（北京航空航天大学）
- Southwest Jiaotong University（西南交通大学）
- Max-Planck-Institut für Sonnensystemforschung（马克斯·普朗克太阳系统研究所）
- Kyung Hee University（庆熙大学）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究利用表面磁通输运模型成功重现太阳轨道器SO/PHI-HRT的极区磁场观测，表明特定子午流廓线调控向极输运，为太阳大尺度子午流提供新约束。
AI中文摘要：
太阳极区磁场在预测太阳活动周强度方面发挥着基础性作用，并决定了日球层磁场的全球结构。太阳轨道器（Solar Orbiter）搭载的偏振与日震成像仪的高分辨率望远镜（SO/PHI-HRT）提供了前所未有的太阳极区观测，因为太阳轨道器目前可达高达±17°的日面纬度，比近黄道面观测可及的纬度高出约10°。利用这些观测进一步检验表面磁通输运模型，我们成功模拟了SO/PHI-HRT的观测结果，重现了两个极区经向平均径向磁场的纬度分布。这一结果是通过采用WangRH2026提出的子午流廓线实现的，该廓线还重现了太阳活动周25期间SDO/HMI观测到的轴向偶极强度演化、磁蝴蝶图和高纬磁场。我们进一步将该廓线的模拟与采用两个具有不同峰值纬度的代表性子午流廓线的模拟进行了比较。后者未能重现观测到的高纬和极区磁场。比较表明，子午流廓线强烈调控向极磁通输运及由此产生的极区磁场演化。峰值纬度更高的廓线产生更强的磁通涌浪，以及更强且更集中的极区磁场。这些结果为太阳大尺度子午流提供了新的约束。
英文摘要：
The solar polar field plays a fundamental role in predicting solar-cycle strength and determines the large-scale structure of the heliospheric magnetic field. The High Resolution Telescope of the Polarimetric and Helioseismic Imager aboard Solar Orbiter (SO/PHI-HRT) provides unprecedented observations of the solar polar regions, as Solar Orbiter currently reaches heliographic latitudes of up to $\pm17^\circ$, about $10^\circ$ higher than those accessible from near-ecliptic observations. Using these observations to further test surface flux transport models, we present a successful simulation of the SO/PHI-HRT observations, reproducing the latitudinal profiles of the longitudinally averaged radial magnetic field in both polar regions. This result is achieved using the meridional-flow profile proposed by \citet{WangRH2026}, which also reproduces the evolution of the axial dipole strength, magnetic butterfly diagram, and high-latitude magnetic fields observed by SDO/HMI during Solar Cycle 25. We further compare simulations using this profile with simulations employing two representative meridional-flow profiles characterized by different peak latitudes. The latter fail to reproduce the observed high-latitude and polar fields. The comparison demonstrates that the meridional-flow profile strongly regulates poleward flux transport and the resulting polar-field evolution. Profiles peaking at higher latitudes produce stronger flux surges, and stronger and more concentrated polar fields. These results provide new constraints on the large-scale solar meridional flow.
