---
abstract: 'Using spaceborne particle and gamma-ray detection and radio diagnostics
  we study solar energetic particle (SEP) production in the 1996 July 9 event. This
  event is associated with an impulsive soft X-ray flare (9:10 UT) and a coronal mass
  ejection (CME). In a global classification the event is considered as mixed- impulsive.
  A sequence of acceleration processes is identified, starting early in the flare
  impulsive phase and continuing throughout the period when the CME propagated up
  to several R$_solar$ above the photosphere: (1) Gamma-ray, hard X-ray and cm-wave
  emitting particles seen during the flare impulsive phase in the low corona had no
  counterpart at the Solar and Heliospheric Observatory (SoHO) spacecraft. (2) Electrons
  accelerated at a coronal shock wave were revealed by decimetric- to-metric type
  II radio emission and by simultaneous radio signatures of beams traveling to 1 AU.
  (3) Mildly relativistic (>=250 keV) electrons detected by SoHO did not correspond
  to these shock-accelerated populations, but to later mainly impulsive injection
  which was associated with radio brightenings over a large range of coronal altitudes.
  (4) Energetic protons detected by SoHO were accelerated during about 100 min after
  the flare impulsive phase with a gradually evolving production profile that bore
  some similarity with the time profile of broadband metric (type IV) emission. (5)
  While all other particle signatures decayed, a second period of interplanetary proton
  production took place >=2 hours after flare onset. The first, 100 min period of
  SEP acceleration, post-impulsive phase coronal acceleration, is definitely dominant
  in mildly relativistic electrons. Two acceleration periods nearly equally contribute
  to the production of \raisebox-0.5ex\textasciitilde 20 MeV protons. However, the
  second period is more productive in low energy, \raisebox-0.5ex\textasciitilde
  1 MeV, protons. The timing of the SEP injections indicates that neither the impulsive
  flare acceleration in the low corona nor the interplanetary CME at >= 10 R$_solar$
  are the main sources of the high-energy particles observed onboard SoHO. We suggest
  that various acceleration processes related to the reconfiguration of the corona
  in the course of the flare and CME lift-off contribute to the interacting and escaping
  particle populations, with different signatures at different energies and in different
  species.'
adsnote: Provided by the SAO/NASA Astrophysics Data System
adsurl: https://ui.adsabs.harvard.edu/abs/2000A&A...360..729L
authors:
- T. Laitinen
- K. -L. Klein
- L. Kocharov
- J. Torsti
- G. Trottet
- V. Bothmer
- M. L. Kaiser
- G. Rank
- M. J. Reiner
category: publications
date: '2000-08-01'
draft: false
featured: false
journal: A&A
month: August
pages: 729-741
projects: []
publication: A&A
publication_types:
- '2'
tags:
- 'Sun: corona'
- 'Sun: flares'
- 'Sun: particle emission'
title: 'Solar energetic particle event and radio bursts associated with the 1996
  July 9 flare and coronal mass ejection'
type: ARTICLE
volume: '360'
year: '2000'
---