Flares, CMEs and Interplanetary disturbances
| Monique Pick | |
| FASR workshop, May 23-25 2002 |
"Electron beam observations in the..."
| Electron beam observations in the corona | ||
| CMEs, Shocks and IP disturbances | ||
| CME Development | ||
| Coronal origin of particle events: contribution | ||
| Electron events | ||
| SEP events | ||
| FASR characteristics | ||
| FASR and Space Weather | ||
| Recent results and present limitation | ||
| Perspective with FASR | ||
CMEs: Association with eruptive prominences and flares
| % association with flares or prominences (filaments) vary (authors and cycle). | |
| Speeds: few tens up to 2000 km/s. |
| Thermal emission of prominence and surrounding medium | ||
| See Poster C. Marqué | ||
| at 450-150 MHz | ||
| Shocks rarely if never observed | ||
| Outbursts rarely if never observed | ||
| Type I/III Noise storm activity observed | ||
Halo CME May 02 1998
Disk
observations
| CME wrapped by shock | |
| Ahead: piston-driven shock | |
| Flanks: blast wave | |
Simultaneous activity at two far distinct locations
Electron events and coronal origin
| Nearly relativistic collimated electron events | |
| SEP events | |
| Importance of radio imaging and FASR |
Near-relativistic solar electron events
| Haggerty and Roelof 2002 | ||
| ACE/EPAM 4 channels 38-315 keV | ||
| Impulsive beam-like electron events | ||
| Injection with a medium delay of ~8 min after start of EM emission ~1Ro | ||
| Histogram with large dispersion | ||
| Acceleration by coronal shock (V 1000km/s) | ||
Near-relativistic solar electron events
Near-relativistic solar electron events
| ACE/EPAM 10:23:55 UT ( - 13.7 min propagation + 500s) | |
| Signature Ejecta radio 10:21:30 UT 1470 km/s | |
| Near relativistic electrons Injection at 0.3 RS | |
The July 14 2000 Halo CME event
ACE/EPAM and Ulysses/HI-SCALE energetic electrons: 14
July 2000
Comparison with radio observations
| Near scatter-free electrons probes localized regions of the corona identified by imaging radio observations. | |
| Electron Anisotropy agrees in time with appearance of radio sources seen in western quadrant. | |
| D. Maia, M. Pick, S. E Hawkins III,V.V. Formichev, and K. Jiricka, Solar Phys., | |
| issue 1/2, 204, 197-212 2001 . | |
Association between CMEs, ICMEs and shocks
Association between ICMEs, shocks detected near the Earth and CMEs
| Need to cover broad frequency range | ||
| High frequencies | ||
| Filament activation, sigmoids, proton flare regions | ||
| Lowest frequencies ( important to go at ≤100 MHz) | ||
| Shock formation and propagation | ||
| Regions of triggering the event (null point) | ||
| Large scale (3-D) geometry of CMEs, IP disturbances reaching Earth | ||
| Forecast CME reaching Earth and | ||
| Bz at Earth need both High and low frequencies | ||
| Synoptic studies | ||
| Large scale patterns ….. | ||
| Material in flow (Sheeley et al ) at the interface between two coronal holes: sector field with strong gradients, streamer belt distorted (Sheeley and Wang): Regions of instability could be detected in radio | ||
| « Points Pivots » (Martres…) recurrent activity | ||
| Coronal holes: fast solar wind | ||
| Complementary of XUV domain | ||
| Definition of an observing mode for SW | ||
| - We have to improve diagnostics with the existing data | ||
FASR and long term perspective
| Coordination needed for future plans | |