Solar Physics

, Volume 204, Issue 1, pp 165–177

ARTEMIS IV Radio Observations of the 14 July 2000 Large Solar Event

Authors

  • C. Caroubalos
    • Department of InformaticsUniversity of Athens
  • C.E. Alissandrakis
    • Section of Astro-GeophysicsUniversity of Ioannina
  • A. Hillaris
    • Section of Astrophysics, Astronomy and Mechanics, Department of PhysicsUniversity of Athens
  • A. Nindos
    • Section of Astro-GeophysicsUniversity of Ioannina
  • P. Tsitsipis
  • X. Moussas
    • Section of Astrophysics, Astronomy and Mechanics, Department of PhysicsUniversity of Athens
  • J.-L. Bougeret
    • Département de Recherche Spatial, CNRS UA 264Observatoire de Paris
  • K. Bouratzis
    • Section of Astro-GeophysicsUniversity of Ioannina
  • G. Dumas
    • Département de Recherche Spatial, CNRS UA 264Observatoire de Paris
  • G. Kanellakis
    • Thermopylae, O.T.E Inmarsat
  • A. Kontogeorgos
    • Department of ElectronicsTechnological Education Institute of Lamia
  • D. Maroulis
    • Department of InformaticsUniversity of Athens
  • N. Patavalis
    • Department of InformaticsUniversity of Athens
  • C. Perche
    • Département de Recherche Spatial, CNRS UA 264Observatoire de Paris
  • J. Polygiannakis
    • Section of Astrophysics, Astronomy and Mechanics, Department of PhysicsUniversity of Athens
  • P. Preka-Papadema
    • Section of Astrophysics, Astronomy and Mechanics, Department of PhysicsUniversity of Athens
Article

DOI: 10.1023/A:1014277508580

Cite this article as:
Caroubalos, C., Alissandrakis, C., Hillaris, A. et al. Sol Phys (2001) 204: 165. doi:10.1023/A:1014277508580

Abstract

In this report we present a complex metric burst, associated with the 14 July 2000 major solar event, recorded by the ARTEMIS-IV radio spectrograph at Thermopylae. Additional space-borne and Earth-bound observational data are used, in order to identify and analyze the diverse, yet associated, processes during this event. The emission at metric wavelengths consisted of broad-band continua including a moving and a stationary type IV, impulsive bursts and pulsating structures. The principal release of energetic electrons in the corona was 15–20 min after the start of the flare, in a period when the flare emission spread rapidly eastwards and a hard X-ray peak occurred. Backward extrapolation of the CME also puts its origin in the same time interval, however, the uncertainty of the extrapolation does not allow us to associate the CME with any particular radio or X-ray signature. Finally, we present high time and spectral resolution observations of pulsations and fiber bursts, together with a preliminary statistical analysis.

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Copyright information

© Kluwer Academic Publishers 2001