太陽風暴之加速粒子傳輸與電漿特性分析

Solar flares and coronal mass ejections (CMEs) are two major eruptivephenomena of solar storms. The energetic particles and radiations accompaniedwith solar flares and CMEs, as well as the interplanetary magnetic fields andplasmas in specific solar wind structures, can cause severe space weatherevents in solar-terrestrial environment affecting the space explorations andhuman life. It is thus important to characterize the source regions associated withsolar storms for space weather system. In this project, we mainly focus on theType III solar radio bursts which is produced by energetic electrons acceleratedin the solar corona and then transport outward along open magnetic fields to theinterplanetary space. To investigate the roles of magnetic field and plasma on theacceleration and transport effects, we adopt the radio dynamic spectrogram fromParker Solar Probe (PSP) near the Sun together with the solar extreme ultravioletimages and in-situ measurements taken by SDO and STEREO spacecraft. Inaddition, we attempt to clarify the evolution pattern of active regionscorresponding to different types of solar storms from the perspective of plasmaquantities by combining with spectral measurements, multi-wavelengthobservations, and theory. Our research results will provide useful constraint onmodeling and significant information on the warning of severe space weather.The progress of preparing e-Callisto Taiwan station will also be introduced briefly.