Occurrences Rate of Type II and III Solar Radio Bursts at Low Frequency Radio Region 45 − 870 MHz

• Autorzy: Hamidi Z. S. , Shariff N. N. M. , Monstein C.
• Języki publikacji: EN

Abstrakty

EN

Observations of type II and III solar bursts indicate that while type III bursts may appear at any altitude, from the very low corona into interplanetary space, type II solar bursts do not act the same way. This work focuses on recent observations in the radio region on the low frequency region from 45 MHz to 870 MHz. Our analysis employed the accuracy of the daily solar burst measurements of e-CALLISTO network. It was found that solar burst type II explode quite minimum with 1-2 events from 2006 - 2010. However, the data 2011 for solar burst type II increases drastically with 16 events has been recorded. The occurrences of Coronal Mass Ejections (CMEs) events are also increasing up to four times in 2011. Most of the both events can be observed in the range of 150 MHz till 500 MHz. Overall, we can say that the range of photon energy for solar burst type III is between 7.737 x 10^-7 eV to 1.569 x 10^-6 eV. In the case of solar burst type II, the distribution of energy is much smaller with 1.596 x 10^-6 eV to 6.906 x 10^-6 eV. Detailed investigation of solar burst will concern the 2011 data seem to show a significant trend for both types. We showed that the increasing of both solar burst events via years implies directing an increasing of solar activities including sunspot number, solar flare and Coronal Mass Ejections (CMEs) events. It is expected that both types will increase gradually in the beginning of 2014.

Słowa kluczowe

EN

CALLISTO; low frequency; solar burst; type II; type III; solar flare; Coronal Mass Ejections; CMEs

• Wydawca: Przedsiębiorstwo Wydawnictw Naukowych "DARWIN"
• Czasopismo: International Letters of Chemistry, Physics and Astronomy
• Rocznik: 2014
• Tom: Vol. 18
• Strony: 103--112
• Opis fizyczny: Bibliogr. 62 poz., rys., tab.

Twórcy

autor

Hamidi Z. S.

• School of Physics and Material Sciences, Faculty of Sciences, MARA University of Technology, 40450, Shah Alam, Selangor, Malaysia

autor

Shariff N. N. M.

• Academy of Contemporary Islamic Studies (ACIS), MARA University of Technology, 40450, Shah Alam, Selangor, Malaysia

autor

Monstein C.

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

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