论文标题
耀斑事件中太阳大气中声学振荡的频率分布
Frequency Distribution of Acoustic Oscillation in the Solar Atmosphere During Flare Event
论文作者
论文摘要
我们介绍了一项研究的研究，该研究在2015年5月23日观察到的活性区域NOAA 12353中的C 2.3太阳耀斑，揭示了耀斑区域的声波的新特性。本文使用了由Heliosemologicy大型区域进行的空间数据，该数据在真空塔望远镜，大气成像组件以及船上的Helioseissic和磁成像仪上运行的太阳能动态观测站，在本文中使用。首先，使用太阳能振荡的功率谱，我们在火炬事件发生前后确定了主要频率及其位置在七个不同的大气水平上。其次，基于在六个极端紫外线过滤器中进行的AIA观察结果，我们得出了耀斑的差分排放度量（DEM）曲线和DEM图。最后，我们确认了与耀斑直接相关的活动区域中磁场的σ分类。 Our results are as follows: the high-frequency waves (ν>5 mHz) in the photosphere, in both cases, before and after the flare, are generated at the foot-points of the chromospheric loop, while in the chromosphere (Hα line), before the event the power enhancement exhibits for maximum of flare emission, and after the eruption the enhancement by all frequencies is observed only in the post flare loop area.此外，在耀斑具有随机特征之前，孔周围孔中振荡的力量，而在耀斑振荡的力量集中在孔中并在外部削弱。我们得出的结论是，在活动区域中准确检测高频声波可以导致更快，更容易预测高能事件。
We present a study of multi-wavelength observations, of a C 2.3 solar flare in Active Region NOAA 12353, observed on 2015 May 23, which reveal new properties of acoustic waves in the flaring region. The space-, and ground-based data measured by the HELioseismological Large Regions Interferometric Device, operating at the Vacuum Tower Telescope, the Atmospheric Imaging Assembly, and Helioseismic and Magnetic Imager on board the Solar Dynamic Observatory, were used in this paper. First, using power spectra of solar oscillations, we identified the dominant frequencies and their location at seven different atmospheric levels before and after the flare event. Second, based on AIA observations taken in six Extreme Ultraviolet filters, we derived Differential Emission Measure (DEM) profiles and DEM maps of the flare. Finally, we confirm the σ-classification of the magnetic field in the active area, directly related to the flare. Our results are as follows: the high-frequency waves (ν>5 mHz) in the photosphere, in both cases, before and after the flare, are generated at the foot-points of the chromospheric loop, while in the chromosphere (Hα line), before the event the power enhancement exhibits for maximum of flare emission, and after the eruption the enhancement by all frequencies is observed only in the post flare loop area. Moreover, the power of oscillation in the pores surrounding area before the flare has a random character, while after the flare oscillation's power is concentrated in the pore, and weakened outside of. We conclude that the accurate detection of high-frequency acoustic waves in the active regions can lead to faster and easier prediction of high-energy events.
