带状太阳耀斑中准周期脉动非热辐射的成像观测
Imaging Observations of Quasi-Periodic Pulsatory Non-Thermal Emission in Ribbon Solar Flares
摘要：
使用RHESSI和一些辅助观测，我们研究了非热硬X射线（HXR）发射源的空间和时间形态之间的可能联系，这些发射揭示了2003年5月29日和2005年1月19日两个带状耀斑期间的准周期脉动（QPPs）。微波辐射也揭示了相同的准周期性。非热HXR发射源主要位于TRACE和SOHO仪器观测到的耀斑拱圈的足点内。至少有一个源在QPP阶段期间和之后在每个耀斑中系统地移动，这允许通过磁重联过程来检查源的速度和能量释放率。在QPP阶段，这些源主要平行于磁反转线或适当的耀斑带移动，而在QPP之后，这些源的移动稍微改变为更垂直的状态。每个QPP从其自身位置发射。计算结果还表明，速度和能量释放率与计算出的HXR辐射通量没有很好的相关性。微波和热HXR的源位于环形拱圈的顶点附近，并且也不是静止的。几乎所有的QPP和一些尖峰的HXR发射在后QPP阶段揭示了软-硬-软的光谱行为，表明单独的电子加速和注入的行为，而不是调制的发射通量的某些种类的磁流体动力学（MHD）振荡的冕环。在所有的可能性，耀斑的情况下，连续发射的拱廊圈的基础上更可取的解释的意见，虽然我们不能确切地得出结论，是什么机制迫使这些环耀斑。
英文摘要：
Using RHESSI and some auxiliary observations we examine possible connections between spatial and temporal morphology of the sources of non-thermal hard X-ray (HXR) emission which revealed minute quasi-periodic pulsations (QPPs) during the two-ribbon flares on 2003 May 29 and 2005 January 19. Microwave emission also reveals the same quasi-periodicity. The sources of non-thermal HXR emission are situated mainly inside the footpoints of the flare arcade loops observed by the TRACE and SOHO instruments. At least one of the sources moves systematically both during the QPP-phase and after it in each flare that allows to examine the sources velocities and the energy release rate via the process of magnetic reconnection. The sources move predominantly parallel to the magnetic inversion line or the appropriate flare ribbon during the QPP-phase whereas the movement slightly changes to more perpendicular regime after the QPPs. Each QPP is emitted from its own position. It is also seen that the velocity and the energy release rate don't correlate well with the flux of the HXR emission calculated from the sources. The sources of microwaves and thermal HXRs are situated near the apex of the loop arcade and are not stationary either. Almost all QPPs and some spikes of HXR emission during the post-QPP-phase reveal the soft-hard-soft spectral behavior indicating separate acts of electrons acceleration and injection, rather than modulation of emission flux by some kinds of magnetohydrodynamic (MHD) oscillations of coronal loops. In all likelihood, the flare scenarios based on the successively firing arcade loops are more preferable to interpret the observations, although we can not conclude exactly what mechanism forces these loops to flare up.
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