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Observations Morphology Quantitative properties Underlying Physics Aly-Sturrock limit

Observations Morphology Quantitative properties Underlying Physics Aly-Sturrock limit Present Theories/Models. Coronal Mass Ejections (CME). S. K. Antiochos, NASA/GSFC. Observations Morphology Quantitative properties Underlying Physics Aly-Sturrock limit Present Theories/Models

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Observations Morphology Quantitative properties Underlying Physics Aly-Sturrock limit

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  1. Observations Morphology Quantitative properties Underlying Physics Aly-Sturrock limit Present Theories/Models Coronal Mass Ejections (CME) S. K. Antiochos, NASA/GSFC

  2. Observations Morphology Quantitative properties Underlying Physics Aly-Sturrock limit Present Theories/Models Rules of the Lecture Road Tailgate! Backseat Drive! Coronal Mass Ejections (CME) S. K. Antiochos, NASA/GSFC

  3. LASCO C3 Observations of Outer Corona

  4. LASCO C3 Observations of Outer Corona • Coronagraph: 5 – 30 R_s FOV, Cadence ~ 1 hour • Thomson scattering of photospheric white light • I ~ ∫ n_e dl • Observe solar wind structures • V ~ 400 km/s • ~ 3 CMEs/day • Some with V > 1,000 km/s • C_s ~ 104.2 T1/2 ~ 100km/s • V_A ~ 1011.3 B n-1/2 ~ 100km/s • Therefore, must have IP shock • Produces large SEP event, (Jokipii) • Need to see coronal origins

  5. Solar Origins of CMEs • Event directly toward or away from Earth appears as halo • Observe dense structure embedded in ejection

  6. Solar Origins of CMEs

  7. Solar Origins of CMEs • SOHO EIT (EUV telescope), • Observe Fe XII 195A line formed at T ~ 1.5 MK • I ~ ∫ n_e n_i G(T) dl • NOTE!! Bright means high density at a particular T; Dark does not mean lack of material • Cadence ~ 12 min • Resolution ~ 1,500 km • Ejection of filament and formation of bright flare loops associated with CME • Filament ejection much faster than coronal evolution • All CMEs/flares associated with a filament channel

  8. Filament Properties 10/02/00 observations by EIT/SOHO and Kitt Peak • Always lie above photospheric polarity inversion line • Fairly common, ~ 50 % coverage, both active & quiet • Origin is one of the outstanding problems in solar physics

  9. Filament Ejection and Flare

  10. Solar Origins of CMEs • TRACE (EUV telescope) observations of 06/16/2005 event • Observe Fe XIX 171A line formed at T ~ 1.0 MK • Very high cadence < 1 m, and resolution ~ 700 km • Cool (< .01 MK) dense prominence/filament lying below coronal loops (seen in absorption) • Loop height ~ 50 Mm, filament height < 5 Mm • But note, grav. scale height H_g ~ 103.7 T cm • Loop plasma supported by its internal pressure, but prominence plasma must be supported by magnetic field • Field must be horizontal (or concave up) in filament • Coronal loops open and reform during ejection • Clearly, magnetically driven

  11. Recap of CME Morphology • “Typical” event consists of 3 components: • Ejection of coronal magnetic field and mass • Ejection of filament/prominence field and mass • Heating of > 10MK flare coronal loops and acceleration of flare particles (Krucker) • Strength of each component can vary between events, but all are present to some degree • How are they related? • What is role of photosphere?

  12. Role of Photosphere

  13. Role of Photosphere • Filament overlies polarity inversion line (PIL) – low lying • Filament field strongly non-potential (large free energy) • Only place in corona where field observed to have high stress! • Photospheric B-field does not evolve during eruption • Energy buildup slow compared to eruption – 1 km/s Relation of CME Components: • Filament rises before onset of flare heating • Timing wrt CME onset not clear

  14. CME Quantitative Properties • For large event: M ~ 1016 gm, V ~ 1,000 km • E ~ 1032 ergs, t ~ 103 s, Power ~ 1029 ergs/s • L ~ 1010 cm, W ~ 109 cm, F ~ 1010 ergs/cm2/s • Poynting flux ~ EBV, if B ~ 103 G, V ~ 10.5 km/s – much larger than photospheric VA • note that F ~ 103 active region heating – also much larger than chromospheric heating • Plasma plays negligible role in energetics • active region: T ~ 10 6.5 K, N ~ 10 10.5 /cm3, EG ~ 10 ergs/cm3 • B ~ 10 2.5 G, EB ~ 10 3.5 ergs/cm3 • also gravitational potential energy, M gsun H ~ EG << EB

  15. Basic CME Scenario • CME/eruptive flare due to explosive release of magnetic energy stored in corona • For some reason, both low-lying filament channel field and overlying coronal field lose equilibrium and expand outward at Alfvenic speeds • Closing and relaxation of opening field lines produces flare heating and particle acceleration • Rapid drop-off of VA with height produces IP shock, V ~ r-3

  16. Basic CME Cartoon (Courtesy, T. Forbes) - +

  17. Closest terrestrial analogy is volcano Disruption of force balance between upward push and downward pull Fast removal of downward pull results in supersonic expansion On the Sun, this must all be done with smoke and magnetism Filament channel field provides upward push and free energy Overlying coronal field provides downward pull But field lines cannot break!! Underlying CME Physics

  18. Pre-CME Force Balance Consider Lorentz force of filament channel and overlying field: J x B = ( x B) x B = - (B2/2) + (B·) B = - ┴(B2/2) + B2 (iB·) iB magnetic pressure magnetic tension Force-free sheared dipole Dipole field

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