1 / 12

M. Pick, D. Maia, S.J. Wang, A. Lecacheux, D. Haggery, S. E. Hawkins COSPAR 2002

Solar Origin of energetic particle events Near-relativistic impulsive electron events observed at 1 AU. M. Pick, D. Maia, S.J. Wang, A. Lecacheux, D. Haggery, S. E. Hawkins COSPAR 2002. CONTEXT. Association with radio type III bursts (Lin, 1981) In-situ observations IP type III 2-20 KeV

davin
Download Presentation

M. Pick, D. Maia, S.J. Wang, A. Lecacheux, D. Haggery, S. E. Hawkins COSPAR 2002

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Solar Origin of energetic particle eventsNear-relativistic impulsive electron events observed at 1 AU M. Pick, D. Maia, S.J. Wang, A. Lecacheux, D. Haggery, S. E. Hawkins COSPAR 2002

  2. CONTEXT • Association with radio type III bursts (Lin, 1981) In-situ observations IP type III 2-20 KeV • Above 25-50 keV • Release often delayed up to 30 min • Krucker et al., 1999: ¾ delayed events associated EIT wave without radio signature 2classes Role of the moving wave front? Triggering or acceleration? • Haggerty et al.: 2001 Acceleration by CME driven shock and injection at about 1Rs • Coronal sites of acceleration • Magnetic restructuring during CME development (Buttighoffer et al. 1996 Maia et al., 1999, 2001; Pojholainen et al., 2001: Klein et al., 2001)

  3. DATA ANALYSISEPAM/ACE 38-315 keV(Haggerty and Roelof, 2001) 18 February 2002 Pitch angle distribution strongly collimated along IMF At Sun: Intensity maxima no dispersed, scatter- free propagation

  4. DATA ANALYSISCoronal and IP Radio signatures • Wide spectral coverage • Radio source (dm-m) • 5 /11events: complex evolution (spectral, spatial and temporal) WIND DAM 09:28 NRH 18 February 2000

  5. Radio signatures and CME V=898 (± 18) km/s t1Rs =09:06 ± 3min UT NRH: 09:19 UT + DAM • Source of electrons in region of interaction, • First shock is the triggering agent ( 1400 km/s) • Importance of the wide spectral range (Klassen, 01)

  6. May 31, 1999Coronal and IP Radio signatures • Source of electrons associated with long duration stationary storm in corona. Vicinity of one CME leg (Kerdraon et al., 1983). Access to IP medium • Electrons produced during magnetic reconnection during newly formed streamers? (Kahler and Hundhausen, 1992)

  7. May 01, 2000 is not a CME event Radio ejecta 1470 km/s V=1335 ± 70 km/s Radio ejecta Electrons

  8. CONCLUSIONS • Radio signatures found for the 5 « delayed events » • Source of quasi-relativistic electrons associated with reconfiguration of coronal magnetic field during flare/CME events • Present study suggests two kinds with distinct radio signatures • Interaction with some triggering disturbance ( coronal wave, bow shock,….) Consistency with Krucker et al., 1999 • Magnetic reconfiguration (post event, long duration). Evidence that electrons escape • Altitude of this region highly variable from one event to the other one • Opening of the magnetic field during CME development • Importance of wide spectral and imaging coverage

  9. Energetic electron beam events November 28 1997 WIND/WAVES NRH E-W plot Three similar radio events located on the western limb. Each event includes two successive type III groups separated by 4 or 5 minutes D. Maia, M. Pick, S. E. Hawkins, S. Krucker, The Astrophys., 500, 1058, 2001

  10. 04 April 2000 Electron injection

  11. Near-relativistic solar electron events ACE/EPAM 13:46:32 UT ( - 13.7 min propagation + 500s) Signature Ejecta radio13:40 UT750 km/s Near relativistic electrons Injection at 0.42 RS (~15 min delay if onset of EM radiation, no estimate of V shock)

  12. Near-relativistic solar electron events ACE/EPAM 10:23:55 UT ( - 13.7 minpropagation + 500s) Signature Ejecta radio 10:21:30 UT 1470 km/s Near relativistic electrons Injection at 0.3 RS 1470 km/S

More Related