AI 中文总结
该研究通过修改MAGNUS代码开展2.5维双流体磁重联模拟，发现带电-中性粒子碰撞驱动太阳色球层磁重联增强，升温18%至110%，能量释放达10²²至10²³。
AI 中文摘要
磁重联将存储的磁能转化为动能、热能和辐射。尽管在完全电离等离子体中已被广泛研究，但观测表明，电离和复合也会通过改变局域等离子体电阻率并提供额外加热通道发挥作用。本研究针对部分电离的太阳色球层中的磁重联展开研究，分析其形态与能量释放，重点关注弹性碰撞、电离及复合过程。原用于欧姆电阻率和热传导计算的MAGNUS代码被修改，以处理弹性与非弹性碰撞；模拟采用含双流体效应（带电粒子+中性粒子）的2.5维电阻磁流体力学模型，适配碰撞项描述的相互作用，并实现混合显式-隐式格式以应对这些项的刚性。模拟针对三种磁场强度开展：100 G、110 G和120 G，对应宁静太阳条件下低至中色球层的环境。研究发现，重联使等离子体组分升温18%至110%；尽管等离子体β值仅小幅上升，但能量释放大幅增长，表明带电粒子-中性粒子碰撞（而非仅β值或可用磁能）驱动了增强的重联。此外，电离与复合在温度峰值区域（尤其是粒子加速处）最为显著；时间分析得到的最大重联率分别为0.226、0.253和0.279。最后，能量方面，在0.4×0.01×0.4 Mm³的色球层体积内，释放的能量范围为10²²至10²³。
英文摘要
Magnetic reconnection converts stored magnetic energy into kinetic energy, heat, and radiation. While extensively studied in fully ionized plasmas, observations show that ionization and recombination also play a role by modifying the local plasma resistivity and enabling additional heating channels. This study examines magnetic reconnection in the partially ionized solar chromosphere, analyzing its morphology and energy releases with attention to elastic collisions, ionization, and recombination. The MAGNUS code, originally built for ohmic resistivity and heat transfer, was modified to handle elastic and inelastic collisions. The simulations are 2.5D resistive MHD with two-fluid effects (charged + neutrals), adapted to handle interactions via these collision terms. A mixed explicit-implicit scheme was implemented to manage the stiffness of these terms. Simulations were carried out for three magnetic field strengths: 100~G, 110~G, and 120~G. These values correspond to the low- to mid-chromosphere under quiet-Sun conditions. We found that reconnection heats the plasma components by 18\% to 110\%. Although plasma beta rises only slightly, the energy release grows far more, indicating that charged--neutral collisions, not just beta or available magnetic energy, drive the enhanced reconnection. Furthermore, ionization and recombination become most significant in regions of peak temperature, particularly where particles are accelerated. Maximum reconnection rates from temporal analysis are 0.226, 0.253, and 0.279, respectively. Finally, in terms of energy, our results show that in a chromospheric volume of $0.4 \times 0.01 \times 0.4$~Mm$^{3}$, the energy released ranges from $10^{22}$ to $10^{23}$.
Comments34 pages, 14 figures. Accepted for publication in Solar Physics
