Investigation on a Broken Solar Burst Type II during High Activities in AR1613 on 13th November 2012

Abstract

The present article is an attempt to analyze the solar burst Type II observations based on solar flare and Coronal Mass Ejections (CMEs) events. We choose an intriguing type II radio burst with a velocity of 1193 kms -1 that occurred on 2012 November 13 at 2:04:20 UT. In this case, the study of solar radio burst type III is of paramount importance because of the fact that it helps to gain an insight of generation mechanisms of solar flare and Coronal Mass Ejections (CMEs) phenomena. Here, we have got a reasonably clear idea of the various forms under which the type III continuum emission may appear and potentially form a type II burst. However, in this case, the Type II solar burst only successfully forms a fundamental structure within the first few minute period, but broken suddenly before evolve a harmonic structure. This phenomenon is very interesting to be tackled and study. How the burst suddenly broken is still ongoing research seems the event is very rare and hard to be proved. There are a few questions that cause this unique situation which related to: (i) the intensity and duration of type III burst which also related to the classification of solar flare (ii) the probabilities CMEs to occur during that time and also the factor of the total amount of massive burst that exploded, Thus, we can conclude that the solar burst type III event still tells us an enigmatic characteristic from time to time due to the relationship of energetic particles and streams of particles with coronal magnetic fields and the pattern of Sun activity due to the 24th solar cycle. It might an interesting to study in detail the main factor that caused the Type II solar burst broken. Indirectly, it might because of the very intense of solar flares that make the percentage of energy of solar flare become more dominant rather than the acceleration of particles through the Coronal Mass Ejections. Thus, we realize that the potential energy during this event is higher than the kinetic energy of the particles.

Investigation of Drift Rate of Solar Radio Burst Type II due to Coronal Mass Ejections Phenomenon

“…It is determined by taking the start time to end time and start frequency to the end frequency of the solar burst Type II seen in Figure I. Drift rate of the solar radio burst type II was defined as (equation 1): (1) Where f e is frequency of end time, f s is frequency of start time, t e is end time, t s start time.…”

“…In radio astronomy, solar radio emission the observations of solar bursts by low spectral and spatial resolution instruments can provide the light curve and a crude spectrum of the whole flares and Coronal Mass Ejections which may consist of many distinct sources with different characteristics [1]. Sun contains of ionized gases such as 92.1% of hydrogen gas and 7.8% of helium gas mixed up and held together by its own gravity [2].…”