论文标题
耀斑的白光发射与光球磁场变化之间的统计关系
The Statistical Relationship between White-light Emission and Photospheric Magnetic Field Changes in Flares
论文作者
论文摘要
在太阳能耀斑期间，经常观察到连续发射，也称为白光发射（WLE），磁场的永久变化（$δ{b} _ {\ rm {los}} $）经常观察到。但是他们的关系和确切机制仍然未知。我们从统计学上研究$δ{b} _ {\ rm {los}} $与wle之间的关系，在太阳能磁盘上具有不同强度和位置的75个太阳耀斑中。我们分析了SDO/HMI数据，并确定每个耀斑中的每个像素，如果它显示出wle和/或$δ{b} _ {\ rm {los}} $。然后，我们研究了WLE的出现，强度和空间大小，其对耀斑能量的依赖性以及其与$δ{B} _ {\ rm {los}} $的发生相关性。我们在44/75耀斑和$δ{b} _ {\ rm {los}} $ 59/75耀斑中检测到WLE。我们发现wle和$δ{b} _ {\ rm {los}} $是相关的，它们的位置通常在0-60 \％之间重叠。并非所有位置一致，因此可能表明其起源差异。我们发现，WL区域与Power Law与Flare类有关，并扩展了先前研究的发现，即WLE与Power Law与Flare类相关，也适用于C级耀斑。为了将未解决的（Sun-As-A-Star）WL测量与我们的数据进行比较，我们得出了一种计算黑体假设下此类数据的温度和区域的方法。计算出的未解决的WLE区域有所改善，但仍与解决的耀斑区域不同，约为5-10（以前为10-20），这可以通过各种物理或工具性原因来解释。该方法也可以应用于恒星耀斑以独立确定其温度和区域。
Continuum emission, also called white-light emission (WLE), and permanent changes of the magnetic field ($Δ{B}_{\rm{LOS}}$) are often observed during solar flares. But their relation and their precise mechanisms are still unknown. We study statistically the relationship between $Δ{B}_{\rm{LOS}}$ and WLE during 75 solar flares of different strengths and locations on the solar disk. We analyze SDO/HMI data and determine for each pixel in each flare if it exhibited WLE and/or $Δ{B}_{\rm{LOS}}$. We then investigate the occurrence, strength, and spatial size of the WLE, its dependence on flare energy, and its correlation to the occurrence of $Δ{B}_{\rm{LOS}}$. We detected WLE in 44/75 flares and $Δ{B}_{\rm{LOS}}$ in 59/75 flares. We find that WLE and $Δ{B}_{\rm{LOS}}$ are related, and their locations often overlap between 0-60\%. Not all locations coincide, thus potentially indicating differences in their origin. We find that the WL area is related to the flare class by a power law and extend the findings of previous studies, that the WLE is related to the flare class by a power law, to also be valid for C-class flares. To compare unresolved (Sun-as-a-star) WL measurements to our data, we derive a method to calculate temperatures and areas of such data under the black-body assumption. The calculated unresolved WLE areas improve, but still differ to the resolved flaring area by about a factor of 5-10 (previously 10-20), which could be explained by various physical or instrumental causes. This method could also be applied to stellar flares to determine their temperatures and areas independently.
