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【云台学术报告】2016年8月15日(周一)上午10:30-11:30 Y12会议室
2016-08-09  |  作者:  |  【  】 【打印】 【关闭

【学术报告】
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报告题目:On one of the greatest enigmas in astrophysics: Can MHD waves heat efficiently the solar plasma?

报告人:Robertus Erdelyi

报告人单位:SP2RC, University of Sheffield, England

报告时间:2016年8月15日(周一)上午10:30-11:30

报告地点:Y12会议室

报告语言:英文

报告摘要:

Satellite (e.g. SOHO, TRACE, STEREO, Hinode, SDO and IRIS) and ground-based observations (e.g. DST/ROSA, IBIS, CoMP, SST/CRISP, NSVT) have provided a wealth of evidence of waves and oscillations present in a wide range of spatial, temporal and spectral scales of the magnetised solar atmosphere. Our understanding about *localised* solar magnetic structures has been considerably changed in light of these high-resolution observations. There is plenty of evidence that these structures support the presence of MHD waves. MHD waves not only enable us to perform sub-resolution solar magneto-seismology (SMS) of waveguides but are also potential candidates to carry and damp the necessary non-thermal energy in these localised waveguides. First, we will briefly outline the basic recent developments in MHD wave theory relevant to solar plasma heating focussing on linear waves. Next, we will concentrate on the role of the most frequently studied wave classes, including the Alfven, and slow/fast magneto-acoustic kink and sausage waves frequently observed. The current theoretical (and often difficult) interpretations of the detected solar atmospheric wave and oscillatory phenomena within the framework of MHD will be shown. Their photospheric origin and generation mechanism, how these waves penetrate into the chromosphere, transition region or even into the low corona will be addressed. Last, the latest reported observational findings of potential MHD wave flux, in terms of localised plasma heating, in the solar atmosphere with some surprising results will be discussed, bringing us closer to solve the classical coronal heating problem.

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