Preferences help
enabled [disable] Abstract
Number of results
2016 | 57 | 23-32
Article title

Relativistic Energy Associated with a Moving Fiber Burst Type μIV Associated with The Class A Solar Prominence

Title variants
Languages of publication
The relativistic energy electron emission is found to occur only during proton events. Solar prominences usually occur in loop shape and can last for weeks or months. This event allows us to investigate the electron density and drift rate of solar burst type IV During 21st September 2015. During that time the Sun has the highest number of sunspots. The radio sources responsibly for Ivm appear to expand spherically through the solar corona after eject on y solar flare. This event shows a strong radiation in radio region, but not in X-ray region. This burst intense radio phenomena that follow with solar flares. It has a wide band structure from 1412-1428 MHz. It can be considered as an intermediate f drift burst (IMDs). This fiber burst has a negative drift rate where the drift is interpreted by the group velocity of the whistler-mode waves. Their bandwidth is approximately 2% of the emission frequency. The are accompanied a parallel-drift absorption band in the background continuum radiation. The occurrence of the event is interesting in many aspects which is also in ZSIS site. From the dynamic spectra of the CALLISTO, it can be observed that there a moving type IV burst. This burst appears is single SRBT III for approximately 16 minutes at 708UT till 716UT. This burst duration is longer compared to the other events. It can be considered as a Ivμ because it begins at the same time as the explosive phase of solar flare. The solar optical, radio and X-ray emission associated with these various energetic particle emissions as well as the propagation characteristics of each particle species are examined in order to study the particle acceleration and emission mechanisms in a solar flare. At the same time, the number of particles traveled a given path in reconnecting area falls exponentially with increase of this path because of losses owing to a leaving of particles the acceleration volume due to drifts.
Physical description
  • School of Physics and Material Sciences, Faculty of Sciences, Universiti Teknologi MARA, 40450, Shah Alam, Selangor, Malaysia
  • School of Physics and Material Sciences, Faculty of Sciences, Universiti Teknologi MARA, 40450, Shah Alam, Selangor, Malaysia
  • Academy of Contemporary Islamic Studies (ACIS), Universiti Teknologi MARA, 40450, Shah Alam, Selangor, Malaysia
  • Institute of Astronomy, Wolfgang-Pauli-Strasse 27, Building HIT, Floor J, CH-8093 Zurich, Switzerland
  • [1] M. Stix, The sun: an introduction, (2004).
  • [2] Z. Hamidi, N. Shariff, C. Monstein, Understanding Climate Changes in Malaysia Through Space Weather Study, International Letters of Natural Sciences (2014).
  • [3] J. P. Wild, Smerd S. F. and Weiss, A. A., Ann. Rev. Astron. Astrophysicsv 10 (1972).
  • [4] Z. Hamidi, N. Shariff, C. Monstein, First Light Detection of A Single Solar Radio Burst Type III Due To Solar Flare Event, (2014).
  • [5] J. G. Andrews, J. Inst. Maths. Applic. 15 (1976).
  • [6] G. D. Fleishman, Gary, D. E. & Nita, G. M., ApJ 593 (2003).
  • [7] A. O. Benz, Sol. Phys. 96 (1985).
  • [8] H. T. Classen, & Aurass, H., A & A 384 (2002).
  • [9] A. Shanmugaraju, Y.-J. Moon, K.-S. Cho, M. Dryer & Umapathy S., Sol. Phys. 233 (2006).
  • [10] H. S. Hudson, & Warmuth, A. , ApJ 614 (2004).
  • [11] K. S. Cho, Y.J. Moon, M. Dryer, et al., JGR 110 (2005).
  • [12] K. S. Cho, J. Lee, Y.J. Moon, et al., A & A 461 (2007).
  • [13] S. Pohjolainen, & Lehtinen, N.J., A & A 449 (2006).
  • [14] M. J. Reiner, Krucker, S., Gary, D.E., et al., ApJ 657 (2007).
  • [15] B. Vrˇsnak, Warmuth, A., Temmer, M., et al., A & A 448 (2006).
  • [16] C. Dauphin, N. Vilmer, S. & Krucker, A & A 455 (2006).
  • [17] Y. Liu, Luhmann,, B. J.G., S.D., R.P. & Lin, ApJ 691 (2009).
  • [18] D.M. Rust, D.F. and Webb, Soft X-ray observations of large-scale coronal active region brightenings, Solar Phys. 54 (1977) 403-417.
  • [19] N. Gopalswamy Coronal Mass Ejections and Type II Radio Bursts, in Solar Eruptions and Energetic Particles, Geophysical Monograph Series 165 (2006).
  • [20] N. Gopalswamy, A. Lara, M. L. Kaiser, J. L. Bougeret, Near-Sun and near-Earth manifestations of solar eruptions, J. Geophys. Res. 106 (2001a) 25261-25278.
  • [21] Vrˇsnak.B, H. Aurass, J. Magdalenic, N. Gopalswamy, Band-splitting of coronal and interplanetary type II bursts. I. Basic properties Astron. Astrophys 377 (2001) 321-329.
  • [22] E. Aguilar-Rodriguez, N. Gopalswamy, R.J. MacDowall, S. Yashiro, M.L. Kaiser, A Study of the Drift Rate of Type II Radio Bursts at Different Wavelengths, Solar Wind 11/SOHO, 2005, pp. 393-396.
  • [23] N. Gopalswamy, S. Akiyama, S. Yashiro, Major solar flares without coronal mass ejections, in: N. Gopalswamy, D.F. Webb (Eds.), Universal Heliophysical Processes, 2009a, pp. 283-286.
  • [24] Z. S. Hamidi, Probability of Solar Flares Turn Out to Form a Coronal Mass Ejections Events Due to the Characterization of Solar Radio Burst Type II and III, Scientific Publishing, 2014, pp. 85.
  • [25] Z. Hamidi, N. Shariff, C. Monstein, The Different Between the Temperature of the Solar Burst at the Feed Point of the Log Periodic Dipole Antenna (LPDA) and the CALLISTO Spectrometer, (2014).
  • [26] Z. Hamidi, N. Shariff, C. Monstein, W.W. Zulkifli, M. Ibrahim, N. Arifin, N. Amran, Observation of the Radio Frequency Interference (RFI) at the National Space Centre, Malaysia, International Letters of Natural Sciences (2014).
  • [27] Z. S. Hamidi, Z. Ibrahim, Z. Abidin, M. Maulud, N. Radzin, N. Hamzan, N. Anim, N. Shariff, Designing and Constructing Log Periodic Dipole Antenna to Monitor Solar Radio Burst: e-Callisto Space Weather, International Journal of Applied Physics and Mathematics 2 (2011) 3.
  • [28] Z. S. Hamidi, Z. Abidin, Z. Ibrahim, N. Shariff, C. Monstein, Modification and Performance of Log Periodic Dipole Antenna, International Journal of Engineering Research and Development 3 (2012) 36-39.
Document Type
Publication order reference
YADDA identifier
JavaScript is turned off in your web browser. Turn it on to take full advantage of this site, then refresh the page.