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

• Autorzy: Hamidi Z. S. , Shariff N. N. M. , Monstein C. , Zulkifli W. N. A. W. , Ibrahim M. B. , Arifin N. S. , Amran N. A.
• Języki publikacji: EN

Abstrakty

EN

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.

Słowa kluczowe

EN

sun; low frequency; solar radio; burst; type II; type III; e-CALLISTO

• Wydawca: Przedsiębiorstwo Wydawnictw Naukowych "DARWIN"
• Czasopismo: International Letters of Chemistry, Physics and Astronomy
• Rocznik: 2014
• Tom: Vol. 9
• Strony: 8--15
• Opis fizyczny: Bibliogr. 32 poz., rys., zdj.

Twórcy

autor

Hamidi Z. S.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology

autor

Shariff N. N. M.

• Academy of Contemporary Islamic Studies (ACIS), MARA University of Technology

autor

Monstein C.

• Institute of Astronomy, Wolfgang-Pauli-Strasse 27, Building HIT, Floor J, CH-8093 Zurich, Switzerland

autor

Zulkifli W. N. A. W.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology

autor

Ibrahim M. B.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology

autor

Arifin N. S.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology

autor

Amran N. A.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology

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