Radio frequency interference affecting type III solar burst observations

Monstein³

2014

Self Cite

Solar flare is one of the solar activities that take place in the outermost layer of the corona. Solar flares can heat the material to several million degrees in just a few minutes and at the same time they release the numerous amount of energy. It is believed that a change of magnetic field lines potentially creates the solar flares. The objectives of the study are to identify and compare the types of solar flares (in X-Ray) region and to improve understanding of solar flares. Data are taken from the NOAA website, from the United States Department of Commerce, NOAA, Space Weather Prediction Center (SPWC). Solar radio flux readings were merged together with the three classes and a total of nine graphs were plotted. In illustrating the relationship of solar radio flux and solar flares, it can be explained by studying the range values of flux corresponding to flares values. From this case study, it was found that the minimum value of solar radio flux in order for the flares to occur is equivalent 68 x 10 -22Wm -2 Hz -1 . Thus, whenever the values of solar radio flux are high, there should be a higher number of flares produced by the sun. The overall range of solar radio flux recorded in this study ranging from 68 x 10 -22 Wm -2 Hz -1 to 96 x 10 -22 Wm -2 Hz -1. Observing and collecting data from the Sun and develop our very own new prediction methods will leads the accuracy of the prediction of the behavior of the Sun more precisely.

Section: Experimental Setup and Observationmentioning

confidence: 99%

Statistical Study of Nine Months Distribution of Solar Flares

Monstein³

2014

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“…This range has a very minimum interference at Blein, Switzerland site [53,54]. Selected the data from the 150 MHz till 900 MHz region seems this is the best range with a very minimum of Radio Frequency Interference (RFI) [54,55,56,57,58]. The next section will highlight the detailed analysis of solar flares in an X-ray and radio region to evaluate the distribution of high and low energy [41].…”

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.

“…Radio telescopes with antenna systems allow determination of the direction of the source of the solar burst radiation. The main detector, Compound Astronomical Low-frequency, Low-cost Instrument for Spectroscopy Transportable Observatories (CALLIISTO) system is used in obtaining a dynamic spectrum of solar radio burst data [12,13]. At our site, we have constructed the Log Periodic Dipole Antenna (LPDA) and this system was mounted on the top of the rooftop of National Space Centre (ANGKASA) building at Sg.…”

Section: Experimental Setup and Observationmentioning

confidence: 99%

An Analysis of Eruption of the Sun Detected by Solar Radio Burst Type I

Arifin

et al. 2015

Self Cite

Type I solar burst were identified based on data recorded by CALLISTO BLEIN, Switzerland in the period of 17 th of January, 2011. Solar Radio Burst Type I is one of the main type of solar burst which is believed to provide a diagnostic of electron acceleration in the corona. This noise storm burst is associated with emerging and growing active regions and last from hours to days. It can be observed that solar radio burst type I is formed within four minutes, although the number of sunspots is just 15. The results of the recent time indicate that Sunspot group 1147 has been mostly quiet since it rounded the eastern limb, but previous week's far side activity shows it is capable of significant eruptions. In 2011, only one day has been detected with spotless day, which means that it is about 7% of overall cases. Probabilities for significant disturbances in Earth's magnetic field are given for three activity levels: active, minor storm, severe storm. From the current conditions in the space weather website on 16th January 2011 that is the first event was shown that the solar wind occurred with a speed of 433.2 km/second while its density about 3.2 protons/cm3. Besides the solar wind, X-ray solar flare with 6 hours maximum: B1 at 1846 UT and 24 hours: B2 at 1544 UT were detected. While type I seem to be an indicator of pre-solar flare and CMEs, on the observational analysis, we could not directly confirmed that this is the only possibility, and we need to consider other processes to explain in detailed the injection, energy loss and the mechanism of the acceleration of the particles. . We could conclude one active region will not produce a huge explosion of solar phenomena.