当前位置: X-MOL 学术Astron. Astrophys. Rev. › 论文详情
Our official English website, www.x-mol.net, welcomes your feedback! (Note: you will need to create a separate account there.)
Solar flares at submillimeter wavelengths
The Astronomy and Astrophysics Review ( IF 25.8 ) Pub Date : 2013-03-23 , DOI: 10.1007/s00159-013-0058-3
Säm Krucker , C. G. Giménez de Castro , H. S. Hudson , G. Trottet , T. S. Bastian , A. S. Hales , J. Kašparová , K.-L. Klein , M. Kretzschmar , T. Lüthi , A. Mackinnon , S. Pohjolainen , S. M. White

We discuss the implications of the first systematic observations of solar flares at submillimeter wavelengths, defined here as observing wavelengths shorter than 3 mm (frequencies higher than 0.1 THz). The events observed thus far show that this wave band requires a new understanding of high-energy processes in solar flares. Several events, including observations from two different observatories, show during the impulsive phase of the flare a spectral component with a positive (increasing) slope at the highest observable frequencies (up to 405 GHz). To emphasize the increasing spectra and the possibility that these events could be even more prominent in the THz range, we term this spectral feature a “THz component”. Here we review the data and methods, and critically assess the observational evidence for such distinct component(s). This evidence is convincing. We also review the several proposed explanations for these feature(s), which have been reported in three distinct flare phases. These data contain important clues to flare development and particle acceleration as a whole, but many of the theoretical issues remain open. We generally have lacked systematic observations in the millimeter-wave to far-infrared range that are needed to complete our picture of these events, and encourage observations with new facilities.

中文翻译:

亚毫米波长的太阳耀斑

我们讨论了在亚毫米波长下首次系统观测太阳耀斑的意义,这里定义为观测波长短于 3 毫米(频率高于 0.1 THz)。迄今为止观察到的事件表明,该波段需要对太阳耀斑中的高能过程有新的认识。几个事件,包括来自两个不同天文台的观测结果,表明在耀斑的脉冲阶段,光谱分量在最高可观测频率(高达 405 GHz)处具有正(增加)斜率。为了强调增加的光谱以及这些事件在太赫兹范围内可能更加突出的可能性,我们将此光谱特征称为“太赫兹分量”。在这里,我们回顾了数据和方法,并批判性地评估了这种不同成分的观察证据。这个证据很有说服力。我们还审查了对这些特征的几种建议解释,这些解释已在三个不同的耀斑阶段报告。这些数据包含整体上耀斑发展和粒子加速的重要线索,但许多理论问题仍然悬而未决。我们通常缺乏在毫米波到远红外范围内完成我们对这些事件的描述所需的系统观测,并鼓励使用新设施进行观测。
更新日期:2013-03-23
down
wechat
bug