Preferences help
enabled [disable] Abstract
Number of results
2016 | 45 | 2 | 264-275
Article title

The Development of Solar Prominence on 4th September 2015 and the Solar Burst Type III and IV

Title variants
Languages of publication
This article will focus on the solar prominences that occur during the 4th September 2015. On that day, there were two sunspots on the surface of the sun, which were AR2409 and AR2410. These two active regions did not produce any threat for strong flare and thus the solar activity was very low. The prominences that will be focused were both occurred at 0353 UT and 0427 UT respectively. There were minor (G1) geomagnetic storm observed on that day. For solar prominences that occurred at 0353 UT, solar radio burst type (SRBT) IV was detected by CALLISTO spectrometer. From the CALLISTO, two bursts at low intensities with the duration of about 7 minutes for the first burst of 280-320 MHz and 6 minutes for the second burst of 360-430 MHz were observed. For the first burst, energy calculated was between 1.855 x 10 -25 J and 2.12 x 10 -25 J with the drift rate of 0.095 MHz/s. For second burst, the energy obtained was between 2.385 x 10 -25 J and 2.849 x 10 -25 J with the drift rate of 0.194 MHz/s. At 0427 UT, SRBT III was recorded with a frequency of 240-350 MHz with the energy which was obtained between 1.590 x 10 -25 J and 2.319 x 10 -25 J. The drift rate of this type of burst was 0.61 MHz/s. During this event, the solar wind value was 499.3 km/Sec with the proton density of 15.1 protons/cm3.
Physical description
  • [1] Aschwanden, M., Physics of the Corona, An Introduction. 2004, New York: Springer.
  • [2] Stix, M., The sun: an introduction. 2012: Springer Science & Business Media.
  • [3] Gaizauskas, V., et al., Formation of a solar filament channel. The Astrophysical Journal, 1997. 479(1): p. 448.
  • [4] Mackay, D.H., V. Gaizauskas, and A.R. Yeates, Where do solar filaments form?: Consequences for theoretical models. Solar Physics, 2008. 248(1): p. 51-65.
  • [5] Martin, S.F., Conditions for the formation and maintenance of filaments–(Invited Review). Solar Physics, 1998. 182(1): p. 107-137.
  • [6] Hundhausen, J. and B. Low, Magnetostatic structures of the solar corona. 1: A model based on the Cauchy boundary value problem. The Astrophysical Journal, 1994. 429: p. 876-889.
  • [7] Koutchmy, S., J. Picat, and M. Dantel, A polarimetric study of the solar corona observed during the total eclipse of June 30, 1973 by means of a radial neutral filter. Astronomy and Astrophysics, 1977. 59: p. 349-357.
  • [8] Koutchmy, S., et al., Photometrical analysis of the June 30, 1973 solar corona. Astronomy and Astrophysics, 1978. 69: p. 35-42.
  • [9] Pasachoff, J., et al., Fine structures in the white-light solar corona at the 2006 eclipse. The Astrophysical Journal, 2007. 665(1): p. 824.
  • [10] Saito, K. and E. Tandberg-Hanssen, The arch systems, cavities and prominences in the helmet streamer observed at the solar eclipse, November 12, 1966. Solar Physics, 1973. 31(1): p. 105-121.
  • [11] Tandberg-Hanssen, E. The nature of solar prominences. in Astrophysics and Space Science Library. 1995.
  • [12] Zirker, J., Quiescent prominences. Solar physics, 1989. 119(2): p. 341-356.
  • [13] Pneuman, G., Temperature-density structure in coronal helmets: the quiescent prominence and coronal cavity. The Astrophysical Journal, 1972. 177: p. 793.
  • [14] Bommier, V., et al., Complete determination of the magnetic field vector and of the electron density in 14 prominences from linear polarizaton measurements in the HeI D3 and Hα lines. Solar Physics, 1994. 154(2): p. 231-260.
  • [15] Athay, R.G., et al., Vector magnetic fields in prominences. Solar physics, 1983. 89(1): p. 3-30.
  • [16] Leroy, J., V. Bommier, and S. Sahal-Brechot, The magnetic field in the prominences of the polar crown. Solar Physics, 1983. 83(1): p. 135-142.
  • [17] Heinzel, P., I. Dorotovič, and R.J. Rutten, The Physics of Chromospheric Plasmas: Proceedings of the Coimbra Solar Physics Meeting Held at the University of Coimbra, Coimbra, Portugal, 9-13 October, 2006. Vol. 368. 2007: Astronomical Society of the pacific.
  • [18] Hale, G.E., Solar Prominences , Solar Flares and Coronal Mass Ejections. 2007: p. 1-10.
  • [19] McLean, D.J. and N.R. Labrum, Solar radiophysics: Studies of emission from the sun at metre wavelengths. 1985.
  • [20] Melrose, D., Plasma emission due to isotropic fast electrons, and types I, II, and V solar radio bursts. Solar Physics, 1975. 43(1): p. 211-236.
  • [21] Wild, J., S. Smerd, and A. Weiss, Solar bursts. Annual Review of Astronomy and Astrophysics, 1963. 1: p. 291.
  • [22] Hamidi, Z., et al., Theoretical Review of Solar Radio Burst III (SRBT III) Associated With of Solar Flare Phenomena. International Journal of Fundamental Physical Sciences, 2013. 3: p. 20-23.
  • [23] Hamidi, Z. and N. Shariff, The Propagation of An Impulsive Coronal Mass Ejections (CMEs) due to the High Solar Flares and Moreton Waves. International Letters of Chemistry, Physics and Astronomy, 2014. 14(1): p. 118.
  • [24] Hamidi, Z., N. Shariff, and C. Monstein, First Light Detection of A Single Solar Radio Burst Type III Due To Solar Flare Event. International Letters of Chemistry, Physics and Astronomy, 2014. 11(1): p. 51.
  • [25] Suzuki, S. and G. Dulk, Solar Radiophysics, ed. 1985, DJ McLean & NR Labrum (Cambridge: Cambridge Univ. Press).
  • [26] Dulk, G.A., Type III solar radio bursts at long wavelengths. Radio Astronomy at Long Wavelengths, 2000: p. 115-122.
  • [27] Hamidi, Z.S., 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. International Letters of Chemistry, Physics and Astronomy, 2014. 16: p. 2.
  • [28] Melrose, D., On the theory of type II and type III solar radio bursts. II. Alternative model. Australian Journal of Physics, 1970. 23(5): p. 885-904.
  • [29] Frank, L.A. and D.A. Gurnett, Direct observations of low-energy solar electrons associated with a type III solar radio burst. Solar Physics, 1972. 27(2): p. 446-465.
  • [30] Hamidi, Z., et al., The Beginning Impulsive of Solar Burst Type IV Radio Emission Detection Associated with M Type Solar Flare. International Journal of Fundamental Physical Sciences, 2012. 2: p. 32-34.
  • [31] Hamidi, Z., N. Shariff, and C. Monstein, Disturbances of Solar Eruption From Active Region AR1613. International Letters of Chemistry, Physics and Astronomy, 2014. 13(1): p. 77.
  • [32] Trottet, G. Coronal physics from radio and space observations. in Coronal Physics from Radio and Space Observations. 1997.
  • [33] Fokker, A., Type IV solar radio emission. Space Science Reviews, 1963. 2(1): p. 70-90.
  • [34] Young, C., C. Spencer, and G. Moreton, JA and Roberts. Astrophys. J, 1961. 133.
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.