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2016 | 45 | 2 | 80-91
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An Analysis of Active Regions 11036 Characteristics Leads To Solar Flare Class C7.2 Phenomena

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The solar flares are generated from electromagnetic radiation which is sudden oscillation of the stored energy in the magnetic field of the sun. Flares are categorized according to their brightness as C, M and X, where X is the brightest. The X class flares caused a long-time solar storm and ionospheric radio waves sparkling. The moderate level M class flares mostly effect polar cups and cause short-time radio sparkling. However, the C class flares are weaker than the X and M flares. In this work, we present an active region from the disturbance of magnetic field on the area of the Sun and may lead to powerful event if the magnetic field become stronger. The CALLISTO system network that has been installed in Gauri, India observed data that contain Solar Radio Burst Type II (SRBT II) occurred on 22nd December 2009 at 04:57 UT to 05:02 UT. Five active regions were obtained from online data via internet from the Space Weather website and the Solar Monitor website. All data and information from these sources assist in analyze of the phenomena. The magnetic field and X-ray flux, proton density increase the possibilities that SRBT II observed by CALLISTO network to generate powerful solar flare. When X-ray flux level was at maximum, then solar flare was at peak point. However, solar activity level was low because among of five active regions present, only one C-class flare event occurred. The most active region that contributes this event is an AR11036 with C-class flare.
Physical description
  • [1] O. W. AHMED, R.Q., T. COLAK, and S. IPSON, T. DUDOK DE WIT LPCE/CNRS, Calculate the Energy of Active Regions and Solar Disk on Satellite Images for Real-Time Solar Flare Forecasting. IEEE 2009. 18.
  • [2] V.N. Yurov, A.S.G., V.G. Tyshkevich, The analysis of links between the characteristics of active regions on the Sun and X-flares classes M and X on the GOES scale. Science Direct, 2015. 74: p. 357-362.
  • [3] E. G.‘ Stassinopoulos, G.J.B., D. W. Nakamura, C. A. Stauffer, G. B. Gee, and J. L. Barth, Solar Flare Proton Evaluation at Geostationarv Orbits for Engineering Applications. IEEE TRANSACTIONS ON NUCLEAR SCIENCE, 1996. 43.
  • [4] D.Y. Kolobov, A.A. Chelpanov, A.A. Kochanov, S.A. Anfinogentov, S.A. Chupin, I.I. Myshyakov, V.E. Tomin, Behaviour of oscillations in loop structures above active regions. Science Direct, 2015. 56: p. 2760-2768.
  • [6] B. Ravindra, P.V., Sanjiv Kumar Tiwari, and R. Bhattacharyya, EVOLUTION OF CURRENTS OF OPPOSITE SIGNS IN THE FLARE-PRODUCTIVE SOLAR ACTIVE REGION NOAA 10930. The Astrophysical Journal, 2011. 19.
  • [7] David A. Falconer, R.L.M., Abdulnasser F. Barghouty, and Igor Khazanov, PRIOR FLARING AS A COMPLEMENT TO FREEMAGNETIC ENERGY FOR FORECASTING SOLAR ERUPTIONS. The Astrophysical Journal, 2012. 32: p. 757.
  • [8] Ming Qu, F.Y.S., Ju .ling, Haimin Wang, Solar Flare Tracking Using Image Processing Techniques. IEEE International Conference on Multimedia and Expo (ICME), 2004. 4.
  • [9] Z. S. Hamidi1, N.N.M.S., The Mechanism of Signal Processing of Solar Radio Burst Data in E-CALLISTO Network (Malaysia). International Letters of Chemistry, Physics and Astronomy, 2014(15): p. 30-38.
  • [10] Z. S. Hamidi, N.N.M.S., C. Monstein, Z. A. Ibrahim, Space Weather: The Significance of e-CALLISTO (Malaysia) As One of Contributor of Solar Radio Burst Due To Solar Activity. International Letters of Chemistry, Physics and Astronomy, 2014(7): p. 37-44.
  • [11] Z. S. Hamidi, Z.A.I., Z. Z. Abidin, M. F. Maulud, N. N. Radzin, N. Hamzan, N. M Anim, N. N. M. Shariff, Designing and Constructing Log Periodic Dipole Antenna to Monitor Solar Radio Burst: e-Callisto Space Weather. International Journal of Applied Physics and Mathematics, 2012. 2(3).
  • [12] Z.S. Hamidi, N.N.M.S., Z.Z. Abidin, Z.A. Ibrahim and C. Monstein, Coverage of Solar Radio Spectrum in Malaysia and Spectral Overview of Radio Frequency Interference (RFI) by Using CALLISTO Spectrometer from 1MHz to 900 MHz. Middle-East Journal of Scientific Research, 2012. 12: p. 893-898.
  • [13] Z.S. Hamidi, A., Z.Z, Ibrahim, Z.A,C. Monstein, N.N.M. Shariff, Signal Detection Performed by Log Periodic Dipole Antenna (LPDA) in Solar Monitoring.
  • [14] Zamri Zainal Abidin, N.M.A., Zety Sharizat Hamidi, Christian Monstein, Zainol Abidin Ibrahim, Roslan Umar, Nur Nafhatun Md Shariff, Nabilah Ramlia, Noor Aqma Iryani Aziz, Indriani Sukma, Radio frequency interference in solar monitoring using CALLISTO. NewAstronomy Reviews, 2015. 67: p. 18-33.
  • [15] Joel C. Allred, et al., Radiative Hydrodynamic Models of the Optical and Ultraviolet Emission from Solar Flares. ApJ, 2005. 630(1).
  • [16] Benz, A.O., Solar and Stellar Coronae. 2002: Kluwer Academic Publishers.
  • [17] Aschwanden, M.J., & Güdel, M. , The coevolution of decimetric millisecond spikes and hard X-ray emission during solar flares. ApJ, 1992. 401(2): p. 736-753.
  • [18] Fleishman, G.D., Gary, D. E., & Nita, G. M., ApJ, 2003. 593.
  • [19] Benz, A.O., Sol. Phys., 1985. 96(357).
  • [20] Mandrini, C.H., et al., Quasi-separatrix layers in solar flares. II. Observed magnetic configurations. Astron. Astrophys., 1991. 325: p. 305-317.
  • [21] D. Herdiwijaya. On the relation of type II solar radio burst with X-ray flares and Coronal Mass Ejections (CMEs) during year 2004-2009. in Proceedings of the Third International Conference on Mathematics and Natural Sciences (ICMNS 2010). 2010. Bandung Indonesia.
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