Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
复制标题
DOI：
10.3847/1538-4357/acf9eb
复制
发表时间：
2023-09
期刊：
影响因子：
--
通讯作者：
A. Kosovichev;V. Sadykov;J. Stefan
中科院分区：
文献类型：
--
作者：
A. Kosovichev;V. Sadykov;J. Stefan
太阳动力学观测台的日震磁成像仪（HMI）在2022年5月10日的X1.5耀斑期间观测到第25太阳周期的第一次重大地震事件。我们对地震光球源进行了详细的光谱偏振分析，使用从HMI线性和圆偏振滤光图重建的fei 6173 Å线的Stokes剖面。结果表明，连续辐射的快速变化具有快速增长和较慢的衰减，持续时间为3-4分钟，与Wind航天器上的Konus仪器观测到的硬x射线脉冲时间一致。线核的变化略早于线翼的变化，表明加热从高层开始并向下传播。谱线轮廓变化最显著的特征是4个源中有3个源的谱线核心的瞬态发射，表明下色球层和光球层强烈的脉冲加热。此外，观测到的Stokes剖面的变化反映了震源磁场强度和几何形状的短暂和永久变化。与辐射流体动力学模型的比较表明，脉冲耀斑阶段的物理过程比目前文献中质子和电子束耀斑模型所预测的要复杂得多。
The first significant sunquake event of Solar Cycle 25 was observed during the X1.5 flare of 2022 May 10, by the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory. We perform a detailed spectro-polarimetric analysis of the sunquake photospheric sources, using the Stokes profiles of the Fe i 6173 Å line, reconstructed from the HMI linear and circular polarized filtergrams. The results show fast variations of the continuum emission with rapid growth and slower decay lasting 3–4 minutes, coinciding in time with the hard X-ray impulses observed by the Konus instrument on board the Wind spacecraft. The variations in the line core appeared slightly ahead of the variations in the line wings, showing that the heating started in the higher atmospheric layers and propagated downward. The most significant feature of the line profile variations is the transient emission in the line core in three of the four sources, indicating intense, impulsive heating in the lower chromosphere and photosphere. In addition, the observed variations of the Stokes profiles reflect transient and permanent changes in the magnetic field strength and geometry in the sunquake sources. Comparison with the radiative hydrodynamics models shows that the physical processes in the impulsive flare phase are substantially more complex than those predicted by proton and electron beam flare models currently presented in the literature.