12-20 July 2017
BEXCO
Asia/Seoul timezone
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Contribution

BEXCO - Room F(201/202/203/204)

[SH025] Origins of two extreme solar particle events

Speakers

  • Alexander MISHEV

Primary authors

Co-authors

  • Leon KOCHAROV (Sodankyla Geophysical Observatory / Oulu Unit, University of Oulu, Finland)
  • S POHJOLAINEN (Tuorla Observatory, University of Turku, Finland)
  • M.J. REINER (The Catholic University of America and NASA/Goddard Space Flight Center, USA)
  • Jeongwoo LEE (Department of Physics and Astronomy, Seoul National University, Korea)
  • T LAITINEN (Jeremiah Horrocks Institute, University of Central Lancashire, UK)
  • L.V. DIDKOVSKY (University of Southern California Space Sciences Center, USA)
  • V.J. PIZZO (NOAA Space Weather Prediction Center, USA)
  • Roksoon KIM (Korea Astronomy and Space Science Institute, Korea)
  • A KLASSEN (Institut f"ur Experimentelle und Angewandte Physik, Christian-Albrechts-Universitat, Germany)
  • M. KARLICKY (Astronomical Institute of the Czech Academy of Sciences, Czech Republic)
  • Kyung-Suk CHO (Korea Astronomy and Space Science Institute, Korea)
  • G.A. KOVALTSOV (A.F.Ioffe Physical-Technical Institute, Russia)
  • Ilya USOSKIN (Sodankyla Geophysical Observatory / Oulu Unit, University of Oulu, Finland)
  • Eino VALTONEN (Space Research Laboratory, University of Turku, Finland)
  • Rami VAINIO (Space Research Laboratory, University of Turku, Finland)

Description

Purpose. We analyze the data of multi-wavelength observations of extreme solar particle events. In such events, protons are accelerated to relativistic energies and can cause a significant signal even in the ground-based particle detectors. We consider a pair of extreme particle events, the events of 2 May 1998 and 2 November 2003, to reveal their production scenario and origins at/near the Sun. Methods. Analysis of a relativistic proton event is based on modeling of the particle transport and interaction, from a near-Sun source through the solar wind and the Earth's magnetosphere and atmosphere to a detector on the ground. This allows us to deduce the time profile of the proton source at the Sun and compare it with observed electromagnetic emissions. Results. We find a common scenario for both considered eruptions. The scenario includes the flare's dual impulsive phase, followed by the CME launch, and after that, the late, low-frequency type III radio bursts at the time of the intensified type II radio emission and the relativistic proton injection into the interplanetary medium. Conclusions. The analysis supports the idea that the two considered events start with emission of relativistic protons previously accelerated at the flare and separately at the CME launch, then trapped in large-scale magnetic loops, possibly re-accelerated there by shock and turbulence, and later released by the expanding CME via he CME-induced magnetic reconnection with open field.