Notes

Outline

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

Type III bursts at 169 MHz

Type III bursts: polarisation

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.

Filament/prominence eruption 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

Flare/CME events

Slide 8

Halo CME May 02 1998 Disk observations

Slide 10

CMEs and shocks CME wrapped by shock Ahead: piston-driven shock Flanks: blast wave

Flare/CME events

Slide 13

Slide 14

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

Slide 21

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 .

Slide 23

FASR and Space Weather

Association between CMEs, ICMEs and shocks

Association between ICMEs, shocks detected near the Earth and CMEs

FASR and Space Weather 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

FASR and Space Weather 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