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17年08月:AOGS 2017年会征文
[ 录入者:admin | 时间:2016-12-06 09:56:07 | 作者:武昭 | 来源: | 浏览:1063次 ]

会议时间:201786-11

会议地点:新加坡

征文截止日期:2017215

注册截止日期:2017524

会议网址:http://www.asiaoceania.org/aogs2017/public.asp?page=home.htm

 

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ST12Waves and Turbulence in the Solar Atmosphere and Solar Wind

召集人:李波 Christopher Chen 何建森 Leon Ofman 吴德金

Waves and turbulence are key to a number of key issues in the physics of the solar atmosphere and solar wind. Magnetohydrodynamic (MHD) waves have been found in most, if not all, structures in the Sun’s atmosphere. Aided with MHD wave theory, these measurements are indispensible for inferring the atmospheric parameters difficult to measure directly. Meanwhile, sophisticated theoretical and numerical studies have shed new light on the generation, propagation, and dissipation of various wave modes. Wave-based scenarios have been brought back to the forefront of the key issue of coronal heating. Furthermore, the past two decades have seen remarkable progress in understanding turbulence in the solar wind, thanks to in situ instruments on board such spacecraft as Helios, WIND, Ulysses, ACE, and CLUSTER. In particular, weak turbulence is related to waves. With the emergence of new theories and advanced simulations, these measurements helped better understand how wave-vector anisotropy develops, the nature of turbulence at kinetic scales, how intermittency influences turbulence spectra, and how turbulence shapes particle velocity distributions. The interpretation of these in situ measurements also gives clues to how turbulence evolves in the near-Sun regions. Consequently, significant progress was achieved on the physics of turbulence and its role in heating and accelerating the solar wind from coronal sources out to interplanetary space.

This session solicits contributions on waves and turbulence in the solar atmosphere and solar wind from both observational analyses and theoretical or numerical modeling. This session will help build a unified picture on how waves and turbulence evolve from their sources out to the Earth and beyond. It will also help prepare the community for the upcoming data from Solar Orbiter and Solar Probe Plus. Both missions will be launched in 2018, and both are anticipated to provide measurements impacting the above topics.

 

ST06Origin, Eruption, Propagation and Space Weather Effect of Magnetic Flux Ropes

召集人:宋红强 申成龙 程鑫 胡强

Coronal mass ejections (CMEs) and flares are the most energetic eruptive phenomena in the solar system, which can disturb the interplanetary space environment seriously and influence some high-technology activities of human being. It is believed that the origin and eruption of magnetic flux ropes are closely related with CMEs and Flares, and the flux ropes may lead to strong geo-magnetic storms when they collide with the Earth's magnetosphere. However, it is not a trivial task to identify the flux rope structures and analyze their associated characteristics on the Sun as no reliable measurement of coronal magnetic field is available at the present time. Further, we do not know the detailed propagation process of magnetic flux ropes and induced space weather effect due to limited space exploration resources. Therefore, the origin, eruption, propagation and space weather effect of magnetic flux ropes are not yet adequately addressed. This session solicits contributions focusing on the studies of solar and interplanetary magnetic flux ropes from both observations/laboratory experiments and simulations/theoretical analysis.

 
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