"Chanruangrith Channok,1 David Ruffolo..."

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"Fe/O at IP shocks..."

Spectra and abundances for Nov. 24 2001 IP shock

Why do ESP spectra roll over at ~ 0.1 - 10 MeV/n?  (data - see also: Gosling et al. 1981; van Nes et al. 1985)

Finite-Time Shock Acceleration

We solve the PDE É

Rollover energy (Ec /A)

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Event #3: λ0 = 0.24 AU, α = 0.18

Event #2: λ0 = 0.042 AU, α = 0.10

Event #1: λ0 = 4.0x10-3 AU, α = 0.07

Fe/O ratios

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É but wait Ð thereÕs more! Key processes of interplanetary transport

Pitch-angle transport equation [DR, ApJ Õ95]

"Fitting SEP data"

Magnetic Configurations

Results of fitting GLE data (relativistic solar protons)

Comparison with EM timing

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Thank you for your attention ขอบคุณครับ

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Early observations [Bryant et al. 1962]

Spectral Properties of Heavy Ions Accelerated by Interplanetary Shocks Near 1 AU  M. I. Desai University of Maryland, College Park, MD 20742, USA Co-Authors: G. M. Mason, C. M. S. Cohen, R. A. Mewaldt, M. E. Wiedenbeck, J. E. Mazur, J. R. Dwyer, A. C. Cummings, E. C. Stone, R. A. Leske, R.E. Gold, E. R. Christian, S. M. Krimigis, C.W. Smith, Q. Hu, R. M. Skoug, and T. T. von Rosenvinge

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Upstream and SEP Abundances (Desai et al. 2003  ApJ 558, 1149).

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Fe/O Ratio at shock versus Fe/O ratio upstream (Desai et al. 2003 ApJ vol. 558, 1149)

3. Particle acceleration in space: Shock acceleration

Fundamental mechanism of shock acceleration

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Application to an interplanetary shock:  What if e, r vary with time?

r, e  varying - ODE model

More model parameters ...

Numerical Results

Four Lines of Work: