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2017 | 74 | 181-193
Article title

Heart-shape Active Region 2529 Producing Strong M6.7 class Solar Flare and Gradual Coronal Mass Ejections

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Abstracts
EN
The Centre of the Sun is very important to be study because this layer is where the nuclear reaction will be occurred. During large event pre-flare usually continues a few minutes and followed by impulsive phase about 3 to 10 minutes. Solar storms such as solar flare and Coronal Mass Ejections are frequently occurred on the area of the Sun that have strong magnetic field or known as active region The release of the stored free magnetic energy that probably drives a CME can take many forms including (predominantly) mechanical in the form of an expanding CME and erupting filament, electromagnetic emission in the form of a flare, and also in the acceleration of energetic particles, magnetic field reconfiguration and bulk plasma motion. In this study, the data of active region of the Sun was taken from official website of the Langkawi National Observatory. The image of the active region was observed by using 11-inch Celestron telescope with solar filter. This data confirms that there was a strong M class of solar flare during the day due to eruption of AR 2529 was occurred on 18th of April. From the x-ray flux data also, it can be observed that few days before M6.7 class solar flare occurred, there were several C classes of flare. The evolution of small AR 2529 to a big heart-shape forms an eruption that producing strong M6.7 class of flare and three gradual CMEs. This strong flare caused significant impact around the high technologies of Pacific Ocean by fading the signal at frequencies below 15 MHz.
Year
Volume
74
Pages
181-193
Physical description
Contributors
author
  • Institute of Science, University of Technology MARA, 40450, Shah Alam, Selangor, Malaysia
author
  • Institute of Science, University of Technology MARA, 40450, Shah Alam, Selangor, Malaysia
  • Institute of Science, University of Technology MARA, 40450, Shah Alam, Selangor, Malaysia
  • Institute of Science, University of Technology MARA, 40450, Shah Alam, Selangor, Malaysia
author
  • Institute of Science, University of Technology MARA, 40450, Shah Alam, Selangor, Malaysia
  • School of Physics and Material Sciences, Faculty of Applied Sciences, University of Technology MARA, 40450, Shah Alam, Selangor, Malaysia
author
  • Institute of Astronomy ETH Zurich, Wolfgang-Pauli-Strasse 27, Building HIT, Floor J, CH-8093 Zurich, Switzerland
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Document Type
article
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YADDA identifier
bwmeta1.element.psjd-bfca98e9-def3-410d-868b-11fbf2754c55
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