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International Letters of Chemistry, Physics and Astronomy
Volume 30
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First Light Detection of a Single Solar Radio Burst Type III due to Solar Flare Event

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Abstract:

The eruption mechanism of solar flares and type III are currently an extremely active area of research, especially during the solar cycle is towards maximum. In this case, the total energy of solar burst type III is of the order of solar flare with the explosion of the energy can up to 1015 ergs. The solar flare event is one of the most spectacular explosions that still be on-going study in the solar physics world. This event occurred at 2:000 UT on 15th April 2012 is due to the explosion of the magnetic energy in from the chromosphere and converted into the heating, mass motion and particle acceleration which can be detected by solar radio burst type III. In this work, we will highlight our first light detection of very tiny solar radio burst type III, which has been observed at the National Space Centre, Banting, Selangor detected by the Compound Low Cost Low Frequency Transportable Observatories (CALLISTO) system at 5:53:23. The region of the data is from 150 − 400 MHz in radio region. This burst is drifted from 150 MHz till 260 MHz. It represents a total energy of 6.2035 × 10-7 eV − 1.0753 × 10-6 eV. This fast drift burst is a continuity of the acceleration of the particles which is intermittent, and can be observed since the explosion of the solar flare. Although the burst is very tiny, it is still significant because this burst is the first detection of a single type III burst from our site. Still, the acceleration of the particles can be detected from Earth in the radio region within 3 hours period of observation at the post stage of solar flare.

Info:

Periodical:
International Letters of Chemistry, Physics and Astronomy (Volume 30)
Pages:
51-58
DOI:
10.18052/www.scipress.com/ILCPA.30.51
Citation:
Z. S. Hamidi et al., "First Light Detection of a Single Solar Radio Burst Type III due to Solar Flare Event", International Letters of Chemistry, Physics and Astronomy, Vol. 30, pp. 51-58, 2014
Online since:
Mar 2014
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