太阳“磁场舞蹈”之谜揭开

Core Insights - The research team from the Yunnan Astronomical Observatory has revealed the physical mechanism of oscillatory magnetic reconnection in the solar atmosphere, providing a new theoretical model for understanding the periodic variations of solar activities such as solar flares and coronal mass ejections [1][2] Group 1: Research Findings - The study utilized 2.5D radiative magnetohydrodynamic simulations to reconstruct the process of magnetic flux ropes rising from the convection zone to the atmosphere and reconnecting with the background magnetic field [1] - The simulations indicated that the direction of the current sheet exhibits quasi-periodic reversals, with reversal periods concentrated between 8 to 15 minutes, and the longest reaching 30 minutes, aligning closely with observational data [1] - The research identified that the convection and turbulence in the solar convection zone are key drivers of the oscillatory behavior of magnetic reconnection [2] Group 2: Implications for Solar Activity - The study proposes a new mechanism for oscillatory magnetic reconnection by coupling the dynamics of the convection zone with coronal magnetic reconnection, addressing previous discrepancies between simulation periods and observations [2] - The periodic fluctuations in the magnetic reconnection rate, ranging from 100 to 400 seconds, correlate with the oscillation periods of solar acoustic waves, suggesting a deep connection between internal solar motions and atmospheric activities [2] - This research enhances the understanding of solar activity's periodic pulsations, which could lead to more accurate predictions of solar storms' impacts on Earth [2]