太阳日冕的微波成像光谱

S. Lesovoi, M. Globa, A. Gubin, A. Altyntsev
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引用次数: 0

摘要

对日冕的研究在了解太阳活动方面起着关键作用。微波成像光谱学——测量太阳圆盘上每一点的微波光谱(或图像)——是研究下日冕和色球-日冕过渡区最有前途的方法。太阳微波辐射起源于低日冕和上层色球层,由热电子和非热电子产生。发射方式主要有轫致辐射、回旋共振和回旋同步辐射。太阳安静区辐射主要是轫致辐射,而活跃区辐射主要是由回旋共振机制引起的。回旋同步辐射是由太阳耀斑期间的非热电子产生的。微波发射光谱使我们能够估计活跃区域等离子体的温度和密度。太阳日冕的微波光谱可能是测量平静太阳和瞬态事件的日冕磁场的唯一方法。介绍了新一代太阳射电望远镜——西伯利亚射电日像仪(SRH),并首次在3-24 GHz宽带频率范围内观测到太阳活动。给出了磁场尺度长度的估计方法。利用3 ~ 12ghz频率范围内某有源发射的SRH数据谱估计了标度长度。多面宇宙:理论观测
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Microwave imaging spectroscopy of the solar corona
The study of the solar corona plays a key role in understanding solar activity. Microwave imaging spectroscopy - measuring microwave spectra at every point on the solar disk (or image) - is the most promising method for studying the lower corona and the chromosphere-corona transition region. Solar microwave emission originates in the low corona and in the upper chromosphere and is produced both by thermal and non-thermal electrons. The main types of emission are bremsstrahlung, gyroresonance and gyrosynchrotron emission. The quiet Sun emission is dominated by the bremsstrahlung while the active region emission is due to the gyroresonance mechanism. The gyrosynchrotron emission is generated by non-thermal electrons during solar flares. Microwave emission spectra allow us to estimate the temperature and density of the plasma in active regions. Microwave spectroscopy of the solar corona is perhaps the only method for measuring the coronal magnetic field both for the quiet Sun and for transient events. The Siberian Radioheliograph (SRH), a new generation solar radio telescope, is described, and the first observations of solar activity in the broadband frequency range 3-24 GHz are presented. The estimation of the magnetic field scale length is presented. The scale length was estimated by using the SRH data – spectra of an active region emission in the frequency range 3–12 GHz. The Multifaceted Universe: Theory Observations
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