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[2011-06-01]: Solar magneto-seismology with Alfven waves
2011-05-30  |  作者:  |  【  】 【打印】 【关闭

报告人:  Robertus von Fay-Siebenburgen (Robert Erdelyi)

单位:   University of Sheffield, UK

报告日期: 2011-06-01(星期三)

报告时间: 9:00

地点:    主楼四楼会议室

邀请团队: 抚仙湖太阳基地 & 太阳活动和CME理论研究组

摘要:   The latest satellite missions and ground-based observational campaigns have provided a wealth of evidence of waves and oscillations present in the solar atmosphere. In particular, our
understanding of the structure and dynamics of the solar atmosphere has been considerably changed in light of the high spatial and time resolution observations offered by ground-based (e.g. ROSA, IBIS, CRISP and CoMP) and space-based (e.g. SOHO, TRACE, STEREO, Hinode, SDO, etc.) instruments allowing us to perform sub-resolution magneto-seismology of MHD waveguides in the solar atmosphere (including both open and closed magnetic structures). A review will be given on the current understanding of MHD waves with a particular focus on the examples of such waves in the lower solar atmosphere. Another issue also addressed is the latest status of the sometimes controversial observations of Alfven waves that are expected to be fundamentally important for solar atmospheric dynamics.

Next, an account of our latest theoretical interpretations of the detected wave and oscillatory phenomena within the framework of MHD will be given. The photospheric origin and generation mechanism of peculiar waves (Alfven, sausage an kink) will be addressed numerically, and how these waves can penetrate into the chromosphere, transition region or even into the corona is explained. The role of the magnetic field in the Alfven wave and oscillatory coupling between the solar interior and atmosphere will be addressed briefly.

Finally, in light of our theoretical studies, the presentation will display how the solar magneto-seismology evolved and how the new data on Alfven waves can be used for atmospheric diagnostics, including such important topics as e.g. determining (i) the extent of the force free (or not!) nature of the solar atmosphere, (ii) the geometry, (iii) fine structure, and (iv) even the heating mechanism(s) of coronal loops.

 
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