论文标题
磁性耦合的气氛，快速香肠MHD波和强迫磁场在Sol2014-09-10T17期间重新连接：45 Flare
Magnetically coupled atmosphere, fast sausage MHD waves, and forced magnetic field reconnection during the SOL2014-09-10T17:45 flare
论文作者
论文摘要
我们研究了2014年9月10日的X1.6太阳耀斑期间太阳大气的物理特性和行为。使用小波分离方法分析了稳定的血浆流量和快速香肠MHD波。借助垂直电流近似非无线力场代码研究了磁耦合的气氛和强制磁场重新连接。我们研究了从光球传递的MHD波传递机制，而无需耗散或反射，然后才能到达电晕，并在太阳能电晕上进行了波能分布的机理。 We report a common behavior of (extreme)ultraviolet steady plasma flows (speed of 15.3 -> 10.9 km/s) and fast sausage MHD waves (Alfven speed of 13.7 -> 10.3 km/s and characteristic periods of 1 587 -> 1 607 s), propagating in cylindrical plasma waveguides of the individual atmospheric layers (photosphere -> corona) observed by SDO/AIA/HMI和IRIS太空仪器。分析了通过磁场通量管上方的磁场通量管和磁场的磁场耦合的太阳大气，并分析了波浪强迫的磁场重新连接。在太阳电晕中散发出散布，泄漏和隧道模式的太阳能地震学，尤其是在太阳电晕中，就其对外部大气加热的可能贡献进行了讨论。我们证明了快速香肠MHD波的分散性，可以轻松地产生泄漏和其他模式在波导外传播的模式，而连接各个大气层的磁场通量管可以在活性区域中分布磁场能。这种机制可以有助于冠状能量平衡，并了解我们如何保持冠状加热。
We study the physical properties and behavior of the solar atmosphere during the GOES X1.6 solar flare on 2014 September 10. The steady plasma flows and the fast sausage MHD waves were analysed with the wavelet separation method. The magnetically coupled atmosphere and the forced magnetic field reconnection were studied with the help of the Vertical-Current Approximation Non-linear Force-Free Field code. We studied a mechanism of MHD wave transfer from the photosphere without dissipation or reflection before reaching the corona and a mechanism of the wave energy distribution over the solar corona. We report a common behavior of (extreme)ultraviolet steady plasma flows (speed of 15.3 -> 10.9 km/s) and fast sausage MHD waves (Alfven speed of 13.7 -> 10.3 km/s and characteristic periods of 1 587 -> 1 607 s), propagating in cylindrical plasma waveguides of the individual atmospheric layers (photosphere -> corona) observed by SDO/AIA/HMI and IRIS space instruments. A magnetically coupled solar atmosphere by a magnetic field flux tube above a sunspot umbra and a magnetic field reconnection forced by the waves were analysed. The solar seismology with trapped, leakage, and tunnelled modes of the waves, dissipating especially in the solar corona, is discussed with respect to its possible contribution to the outer atmosphere heating. We demonstrate that a dispersive nature of fast sausage MHD waves, which can easily generate the leaky and other modes propagating outside of their waveguide, and magnetic field flux tubes connecting the individual atmospheric layers can distribute the magnetic field energy across the active region. This mechanism can contribute to the coronal energy balance and to our knowledge on how the coronal heating is maintained.
