SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS

Hilary Cane, Ian Richardson and Tycho von Rosenvinge

Astroparticle Physics Laboratory,NASA/GSFC

PROPOSED STUDIES

• 1 Event Profiles

• 2 Interplanetary Shock Evolution

• 3 Early Component of SEP Events

• 4 Particle Characteristics at In Situ Shocks

From Cane and Lario (2006)

CANE and RICHARDSON

INTERPLANETARY CORONAL MASS EJECTION

SUN

ICME

SHOCK

SHOCK NORMALS IMF

Volkmer and Neubauer 1984

TYPE II

IP TYPE II EVENT

2300 UT 2330 UT

Gopalswamy 2006

m-λ type II

SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS

Hilary Cane, Ian Richardson and Tycho von Rosenvinge

Astroparticle Physics Laboratory,NASA/GSFC

SHOCK ACCELERATION

THIRD PHASE

THREE PHASES OF PARTICLE ACCELERATION

FLARE IMPULSIVE PHASE (FIRST) FLARE LATE PHASE (SECOND)

CME

SHOCK

TWO CONDITIONS for detecting particles in IP space

(1) OPEN FIELD LINES (2) MAGNETIC CONNECTION

LOW FREQUENCY RADIO OBSERVATIONS PROVIDE THE ANSWERS!

ERUPTING LOOP PLUS RECONNECTION = 1st phaseAvailable magnetic energy plus magnetic structure of photosphere and

corona

Very LowNo CME

LowJet

Low/mediumSmall CME

Medium/largeMedium/large CME

No SEP

Open Field Lines?

Yes

No V. Good magneti

c connect

-ion

No

Yes

3He-rich, Fe-rich, He-rich,Electron-rich SEP event

Type III burst

No SEP

Yes

Open Field Lines?

No

Yes

Shock?

Fe-rich, Electron-richSEP event

Type III (and Type II burst)

Connection?

Very good

OK

No

No SEP

Poor

Fe-rich, Electron-rich(possibly 3He-rich He-rich) SEP event

PLUS late Fe-coronal componentType III and Type II burst

Connection?

PoorGood

Yes = 2nd phase

No

Efficient late/extended phase

acceleration?

Open Field Lines?

Aug 14 2002

Yes

No

IMPULSIVE

May 1 2000

No SEP

Sep 17 2002

Connection?

Fe-coronal orFe-poor event

Strong Shock?

Reasonably Fe-rich event

(Type III), type III-l, (II,IV)

Very poor

Fe-rich early component at low and high energies

Fe-coronal/Fe-poor component later(Type III), type III-l, (II,IV)

Good

Connection?

No

Yes

Yes

Sep 15 2001

GRADUAL

Low energy Fe-coronal late event

Possibly type I

ERUPTING LOOP PLUS RECONNECTION = 1st phaseAvailable magnetic energy plus magnetic structure of photosphere and

corona

Open Field Lines?

No SEP

No

Open Field Lines?

Yes = 3rd phase

Jan 8 2002

No

Yes

Passing ShockOr CIR?

No

Aug 9 2001

No

DSF events

Yes

3rd phase + maybe 2nd phase but no 1st phase

Oct 1 2001

Major events

eras MAY 2000

ACE ULEIS / SIS ions

SOHO EPHIN electrons

0.3 - 0.7 MeV0.7 – 1 MeV3 - 6 MeV

SOHO ERNE protons & He

8 – 10 MeV p8 – 10 MeV He26 – 32 MeV p8 – 10 MeV He/p

0.3 – 0.6 MeV/n Fe0.3 – 0.6 MeV/n O10 – 13 MeV/n Fe10 – 13 MeV/n O0.3 – 0.6 MeV/nFe/O

FIRST PHASE ONLYPrompt particles Fe and e - rich

SEPTEMBER 2000

THIRD PHASE ONLY

“DISAPPEARING FILAMENT EVENT”

No prompt particles but W33 location

Delayed Fe-poor increase

CONCLUSIONS

• THREE PHASES OF PARTICLE ACCELERATION

• ALL COMBINATIONS ARE POSSIBLE AND LEAD TO A “ZOO” OF SOLAR ENERGETIC PARTICLE EVENTS