Journal: International Letters of Chemistry, Physics and Astronomy

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Scientific Publishing House Darwin

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2299-3843

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Publications 1 - 6 of 6
  • Investigation of Drift Rate of Solar Radio Burst Type II Due To Coronal Mass Ejections Phenomenon
    Item type: Journal Article
    Zainol, N.H.; Hamidi, Zety S.; Shariff, N.N.M; et al. (2015)
    International Letters of Chemistry, Physics and Astronomy
    The formation of detected solar radio burst type II occurred was captured using Compound Astronomical Low Cost Frequency Spectrometer Transportable Observatory (CALLISTO) system which gives a better resolution of a wonderful image than other countries. The phenomenon was found on 2nd November 2014 at 09:39 [UT] in Switzerland. CALLISTO spectrometer device detects and traces a Coronal Mass Ejections (CMEs) phenomenon that causes the occurrence of the solar burst type II. As it happened, the drift rate of the solar radio burst Type II is calculated and discussed in details. Plasma frequency (fp), Langmuir waves and type II radiation relates each other in the establishment of this phenomenon. This paper presents a study of drift rate selected event of solar radio burst type II based on CMEs. The drift rate at this moment was about 3.2 MHz/s which has low drift rate thus the velocity OF THE CMEs was just about 695 km/s shown from NOAA.
  • An Analysis of a Single Solar Radio Burst Type III and Type II Coronal Mass Ejections Associated to Solar Flare Event
    Item type: Journal Article
    Ali, M.O.; Hamidi, Zety S.; Shariff, N.N.M; et al. (2015)
    International Letters of Chemistry, Physics and Astronomy
    Solar radio burst type III and II is the subject matter that we are focusing on because type II and III burst are seem to have relation to each other. The most common of type III burst is called isolated type III burst which is produced by energetic electron from small scale energy release site on the sun and it is ranging from small bright point to large active region. This stage can be considered as a pre-flare stage that could be a signature of electron acceleration. Nevertheless, the most important is that the nonlinear wave-wave interaction which involving interaction of electrostatic electron plasma that called as Langmuir waves active region radio emissions is believed to be a main subject that relevant with a type III burst. In this study, solar radio bursts are observed by using the CALLISTO spectrometer. The log Periodic Dipole Antenna (LPDA) involved in this search over a broad region centered on the Sun and it covered the range of frequency from 45 MHz-870 MHz and it is connected to the CALLISTO spectrometer. At certain period of time, when the Sun launches billons tones of electrically conducting gas plasma into the space at millions of miles per hours it is assigned that CMEs begin to launches. At this time, the appearance of SRBT III was observed and followed by SRBT II within the time interval of 15 minutes. During flares, large scale of magnetic field structures can be destabilized and be repelled into the interplanetary medium; along with the large mass it contains to form so-called CMEs. Based on the result obtained, the SRBT III is followed by SRBT II which only in short period. During the SRBT II, the solar flare was also appearing and same goes to the CMEs
  • Preliminary Analysis on the Solar Burst Type III and the Effect of the Magnetic Reconnection
    Item type: Journal Article
    Husein, Nurulhazwani; Hamidi, Zety S.; Shariff, N.N.M; et al. (2015)
    International Letters of Chemistry, Physics and Astronomy
    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 Evolution of Unstable 'Beta-Gamma' Magnetic Fields of Active Region AR 2222
    Item type: Journal Article
    Hamidi, Zety S.; Sabri, S.N.U.; Shariff, N.N.M; et al. (2015)
    International Letters of Chemistry, Physics and Astronomy
    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/cm3 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 M-class 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.
  • Determining a Complex Solar Radio Burst Type II on 2nd November 2014 Driven by a Hydra Solar Flare As A Blast Waves
    Item type: Journal Article
    Hamidi, Zety S.; Ibrahim, M.B.; Sharif, N.N.M; et al. (2015)
    International Letters of Chemistry, Physics and Astronomy
    Recent data of a complex solar radio burst type II is analyzed and reviewed. The monitoring of solar radio burst was done by using the Compact Astronomical Low cost, Low frequency Instrument for Spectroscopy and Transportable Observatory (CALLISTO) from BLEIN 7 meter dish telescope at ETH, Zurich in frequency range of 25 until 1000 MHz. During the inspection of the X-ray spectrum, we observed that the C3-category flare was caused by a filament of magnetism, which rose up and erupted between 0400 and 0600 UT. This occurred three hours before the signature of solar radio burst type II. There are some of the material in the filament fell back to the sun, causing a flash of X-rays where it hit the Sun surface. This is a Hydra Flare which occurred without sunspots. On the basis of these results, we suggest that a single shock in the leading edge of the CME could be the source of the multiple type II bursts and support the notion that the CME nose and the CME-streamer interaction are the two main mechanisms able to generate the bursts.
  • An Analysis of Eruption of the Sun Detected by Solar Radio Burst Type I
    Item type: Journal Article
    Hamidi, Zety S.; Shariff, N.N.M; Arifin, L.; et al. (2015)
    International Letters of Chemistry, Physics and Astronomy
    Type I solar burst were identified based on data recorded by CALLISTO BLEIN, Switzerland in the period of 17th 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.
Publications 1 - 6 of 6