1. SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS
Hilary Cane, Ian Richardson and
Tycho von Rosenvinge
Astroparticle Physics Laboratory,
NASA/GSFC

2. PROPOSED STUDIES 1 Event Profiles 2 Interplanetary Shock Evolution
3 Early Component of SEP Events
4 Particle Characteristics at In Situ Shocks

3. From Cane and Lario (2006)

4. CANE and RICHARDSON INTERPLANETARY CORONAL MASS EJECTION ICME SHOCK
SUN
CANE and RICHARDSON

5. SHOCK NORMALS IMF
Volkmer and Neubauer 1984

8. TYPE II
IP TYPE II EVENT
2300 UT UT

9. m-λ type II
Gopalswamy 2006

11. SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS
Hilary Cane, Ian Richardson and
Tycho von Rosenvinge
Astroparticle Physics Laboratory,
NASA/GSFC

12. THREE PHASES OF PARTICLE ACCELERATION
FLARE IMPULSIVE PHASE (FIRST) FLARE LATE PHASE (SECOND)
SHOCK
CME
SHOCK ACCELERATION
THIRD PHASE

13. TWO CONDITIONS for detecting particles in IP space
(1) OPEN FIELD LINES (2) MAGNETIC CONNECTION
LOW FREQUENCY RADIO OBSERVATIONS PROVIDE THE ANSWERS!

14. IMPULSIVE ERUPTING LOOP PLUS RECONNECTION = 1st phase
Available magnetic energy plus magnetic structure of photosphere and corona
IMPULSIVE
Very Low
No CME
Low
Jet
Low/medium
Small CME
Medium/large
Medium/large CME
Shock?
Efficient
late/extended phase
acceleration?
Yes
Yes = 2nd phase
Open Field
Lines?
Open Field
Lines? No No
Yes
Open Field
Lines?
V. Good magnetic connect-ion No No
Yes
No SEP
Connection?
Yes
Connection? No No
Poor
Poor
No SEP
Yes
Good
Very good
No SEP
No SEP OK
Fe-rich, Electron-rich
(possibly 3He-rich He-rich) SEP event
PLUS late Fe-coronal component
Type III and Type II burst
3He-rich, Fe-rich, He-rich,
Electron-rich SEP event
Type III burst
Fe-rich, Electron-rich
SEP event
Type III (and Type II burst)
May
Sep
Aug

15. GRADUAL ERUPTING LOOP PLUS RECONNECTION = 1st phase
Available magnetic energy plus magnetic structure of photosphere and corona
GRADUAL
Strong Shock?
Yes = 3rd phase
Open Field
Lines?
Connection?
Yes
Very poor No
Open Field
Lines? No
Good
Passing Shock
Or CIR?
Aug
Connection?
Jan
Yes
Yes No No
Oct
Fe-coronal or
Fe-poor event
No SEP
Yes
3rd phase + maybe 2nd phase but no 1st phase No
Low energy
Fe-coronal late event
Possibly type I
Reasonably Fe-rich
event
(Type III), type III-l, (II,IV)
Fe-rich early component
at low and high energies
Fe-coronal/Fe-poor component later
(Type III), type III-l, (II,IV)
DSF events
Sep
Major events

16. MAY 2000 FIRST PHASE ONLY SOHO EPHIN electrons 0.3 - 0.7 MeV
Prompt particles Fe and e - rich
SOHO EPHIN electrons
MeV
0.7 – 1 MeV
3 - 6 MeV
SOHO ERNE protons & He
8 – 10 MeV p
8 – 10 MeV He
26 – 32 MeV p
8 – 10 MeV He/p
0.3 – 0.6 MeV/n Fe
0.3 – 0.6 MeV/n O
10 – 13 MeV/n Fe
10 – 13 MeV/n O
0.3 – 0.6 MeV/n
Fe/O
ACE ULEIS / SIS ions
MAY 2000
eras

17. SEPTEMBER 2000 THIRD PHASE ONLY “DISAPPEARING FILAMENT EVENT”
No prompt particles but W33 location
Delayed Fe-poor increase
SEPTEMBER 2000

20. CONCLUSIONS THREE PHASES OF PARTICLE ACCELERATION
ALL COMBINATIONS ARE POSSIBLE AND LEAD TO A “ZOO” OF SOLAR ENERGETIC PARTICLE EVENTS