Oral Presentation

Solar Flares

Author(s): C. Z. Cheng (Institute of Space and Plasma Sciences, National Cheng Kung University)

Presenter: C. Z. (Frank) Cheng (National Cheng Kung University)

It is now accepted that solar flares are produced by the magnetic reconnection process which can accelerate electrons to MeV energy and produce non-thermal emissions such as hard X-ray (HXR), gamma-ray, and millimeter (mm) waves, etc. Solar flares have been extensively observed in HXR, SXR, EUV, and visible lights by telescopes on satellites and on the ground. However, radio emissions in mm and sub-mm wavelength ranges can provide information on gyro-synchrotron emissions produced by high energy electrons near the magnetic reconnection site in the solar corona. The spatial resolution of the present smaller radio telescope systems is too coarse to provide detailed information on where and how electrons are accelerated. Thus, higher resolution flare observation by ALMA should be valuable to understand the physics of how and where electrons are accelerated during flares.