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SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS

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.

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SEP EVENTS AND THE ROLE OF FLARES AND SHOCKS

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  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. INTERPLANETARY CORONAL MASS EJECTION ICME SHOCK SUN CANE and RICHARDSON

  5. SHOCK NORMALS IMF Volkmer and Neubauer 1984

  6. TYPE II IP TYPE II EVENT 2300UT 2330 UT

  7. m-λ type II Gopalswamy 2006

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

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

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

  11. 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 1 2000 Sep 17 2002 Aug 14 2002

  12. ERUPTING LOOP PLUS RECONNECTION = 1st phase Available magnetic energy plus magnetic structure of photosphere and corona GRADUAL Strong Shock? Connection? Open Field Lines? Yes = 3rd phase Yes Very poor No Open Field Lines? No Good Passing Shock Or CIR? Aug 9 2001 Connection? Jan 8 2002 Yes Yes No No Oct 1 2001 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 15 2001 Major events

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

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

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

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