Observation of the Radio Frequency Interference (RFI) at the National Space Centre, Malaysia

Monstein

2014

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The paper describes an investigation of the solar radio bursts of spectral type III due to disturbances of the active region AR 1613. A solar flare occurred on 2012 November 15, between 2:00 UT to 3:30 UT. The sequence images from a burst from our site revealed that although the solar flare is considered moderate, it is still possible to obtain the solar burst type III in a single and group forms within one and half hour. It can easily produce misleading results in terms of nonthermal electron density and magnetic field strength. The burst is originated in the same active region of the solar corona. The C-6 level enhancement was detected in GOES 1.8 a soft X-ray. Based on the results, we suggest that radio wave source motion manifests the displacement of particle sites caused by plasma eruptions. Time variability in the emission may due to the changes in the electron density. The group and individual solar burst type III can be related to the distance travelled before an electron beam becomes unstable to Langmuir waves. In conclusion, the interactions non-thermal electron and magnetic trapping can influence the transporting of electrons and this is still a subject of interest of intense investigation.

Section: Experimental Setup and Methodologymentioning

confidence: 99%

Disturbances of Solar Eruption from Active Region AR1613

Monstein

2014

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“…The CALLISTO spectrometer is a low-cost radio spectrometer used to monitor metric and decametric radio bursts [45,46,47,48,49]. We select the range of 150 MHz till 900 MHz for this data [50,51,52]. This range has a very minimum interference at Blein, Switzerland site [53,54].…”

Section: Solar Flare Observationmentioning

confidence: 99%

Preliminary Analysis on the Solar Burst Type III and the Effect of the Magnetic Reconnection

Husien

et al. 2015

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ABSTRACT. From the data from a BLEIN Callisto site, we aim to provide a comprehensive description of the synopsis formation and dynamics of a a single solar burst type III and magnetic reconnection effect. The data above is the solar radio burst type iii occurred on 10th September 2005 between 05:44 UT till 06:00 UT.This eruption has started since 5:55 UT with a formation of type III solar burst. The wave emission process of solar radio burst type III from magnetic reconnection region in a solar flare were investigated by using a two-dimensional, that are electromagnetic and relativistic particle-in-cell code. The solar radio burst type III initially impose into two plasma populations : background dense plasma and hot electrons that can be generated by the magnetic reconnection process in a solar flare. The conversion of the energy stored in the magnetic field by a process called the magnetic reconnection released the energy in the solar flares and related phenomena. By the launching the e-CALLISTO network, its prove the existence of the magnetic reconnection on the surface of the sun in radio region.

“…The CALLISTO spectrometer is a low-cost radio spectrometer used to monitor metric radio bursts. We select the range of 240 MHz till 360 MHz for this data [20,21,22]. This range has a very minimum interference at KRIM site [23,24].…”

Section: Solar Burst Observationmentioning

confidence: 99%

The Evolution of Unstable 'Beta-Gamma' Magnetic Fields of Active Region AR 2222

Sabri

et al. 2015

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This event allows us to investigate how plasma-magnetic field interactions in the solar corona can produce suprathermal electron populations over periods from tens of minutes to several hours, and the interactions of wave-particle and wave-wave lead to characteristic fine structures of the emission. An intense and broad solar radio burst type IV was recorded by CALLISTO spectrometer from 240-360 MHz. Using data from a the KRIM observatory, we aim to provide a comprehensive description of the synopsis formation and dynamics of a a single solar burst type IV event due to active region AR2222. For five minutes, the event exhibited strong pulsations on various time scales and "broad patterns" with a formation of a group type III solar burst. AR 2222 remained the most active region, producing a number of minor C-Class solar flares. The speed of the solar wind also exceeds 370.8 km/second with 10.2 g/cm 3 density of proton in the solar corona. The radio flux also shows 171 SFU. Besides, there are 3 active regions, AR2217, AR2219 and AR2222 potentially pose a threat for Mclass solar flares. Active region AR2222 have unstable 'beta-gamma' magnetic fields that harbor energy for M-class flares. As a conclusion, we believed that Sun's activities more active in order to achieve solar maximum cycle at the end of 2014.