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Development of Coronal Shocks Seen in the UV John Raymond

Development of Coronal Shocks Seen in the UV John Raymond. Plasma Parameters Measured in the UV. Pre-shock Post-shock n i , n e V shock T e , T i T i , T e

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Development of Coronal Shocks Seen in the UV John Raymond

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  1. Development of Coronal Shocks Seen in the UV John Raymond

  2. Plasma Parameters Measured in the UV Pre-shock Post-shock ni, ne Vshock Te, Ti Ti, Te fp(v), fe(v) Compression < Q> Vplasma Composition <Q> Not Yet Measured All at Once

  3. Diffusive Shock Acceleration Parameters UVCS and STEREO: SEP Physics Seed Particles Diffusion Coefficient,  Thickness of turbulent precursor;  = L V not with UVCS for plausible values of ; CPEX? Shock Angle,  Need model of B field structure; UV may help tune models Injection Efficiency, ε Need to observe at solar maximum n, T, V, width, composition, turbulence and evolution

  4. Pre-CME corona Initial streamer blowout Red & Blue Doppler shift (Raymond et al 2003,ApJ,597) Identifying Shock Waves Magnetic loop has arbitrary T, n, ionization state Anomalously large O kinetic temperature Shock No shock ID Mancuso et al. 2002

  5. UVCS Shock Observations Analyzed so far Date Reference H V n0 Log TO X 06/11/98 Raymond et al. 1.75 1200 1x106 8.7 1.8 06/27/99 Raouafi et al. 2.55 1200 <8.2 03/03/00 Mancuso et al. 1.70 1100 1x107 8.2 1.8 06/28/00 Ciaravella et al. 2.32 1400 2x106 8.1 07/23/02 Mancuso&Avetta 1.63 1700 5x106 8.0 2.2 Modest heights, Modest compression, High TO 5 other shocks not yet fully analyzed (Ciaravella et. al. 2006)

  6. Comparison with Radio Timing & Density agree Velocity; Factor of 2 with UVCS densities; drift rate uncertainty Compression Factor of 2 agrees with radio splitting (Mann et al.) Mancuso et al. 2003

  7. Height of formation: Magnetic Field Strength Many fast CMEs do not show shocks, presumably because the Alfvén speed is even faster. But we may be missing some; Some may not make type II emission. Some may not preferentially heat O. Mancuso & Raymond

  8. Summary Compression is modest; MA ~ 2 Preferential heating of oxygen (Selection?) Weak heating of electrons No detection of seed particles so far

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