Magnetic reconnection of solar flare detected by solar radio burst type III

• Published in: Journal of Physics: Conference Series
• Main Author: Hamidi Z.S.; Shariff N.N.M.; Ibrahim Z.A.; Monstein C.; Wan Zulkifli W.N.A.; Ibrahim M.B.; Arifin N.S.; Amran N.A.
• Format: Conference paper
• Language: English
• Published: Institute of Physics Publishing 2014
• Online Access: https://www.scopus.com/inward/record.uri?eid=2-s2.0-84908042324&doi=10.1088%2f1742-6596%2f539%2f1%2f012006&partnerID=40&md5=d65b90aaa014b7e563f9f9e560e3a350

The Sun is an ideal object of a blackbody with a large and complex magnetic field. In solar activity specifically solar flare phenomenon, the magnetic reconnection is one of the most significant factors of the Sun that can simplify a better understanding of our nearest star. This factor is due to the motion of the plasma and other particles through the convection mechanism inside the Sun. In our work, we will highlight one of the solar burst events that associated with solar flares. This event occurred on 13th November 2012 from 2:00:03 UT till 2:00:06 UT. It peaked with M2.0 solar flare at 2.04 UT. Within short time intervals of about l02 ∼ 103s, large quantities of energy of 1022 ∼ 1026J are emancipated. The changing magnetic field converts magnetic potential energy into kinetic energy by accelerating plasmas in the solar corona. It is believed that the plasma is channelled by the magnetic field up and away from the Sun. It is also accelerated back down along the magnetic field into the chromosphere. In conclusion, we showed that the structure of the solar radio burst type III is an indicator of a starting point of magnetic reconnection. © Published under licence by IOP Publishing Ltd.