Shock-associated energetic proton events at large heliocentric distances

Journal Article · Mon May 01 04:00:00 EDT 1978 · J. Geophys. Res.; (United States)

DOI:https://doi.org/10.1029/JA083iA05p02037· OSTI ID:6931563

Palmer, I D; Gosling, J T

Enhancements of energetic protons (> or approx. =0.5 MeV) in association with forward-reverse shock pairs have been observed at large heliocentric distances. An interpretation of the time profiles of these events is offered in terms of a model of solar wind stream structure. Persistent sweeping of energetic particles by each shock front and their banking-up by reflection lead to the formation of a gradient along field lines upstream of the shocks. The rise (fall) of intensity before (after) the forward (reverse) shock is explained by a gradient in particle density directed along the upstream field lines toward the shock. A marked intensity decrease between the two shocks is interpreted in the same fashion as being due to parallel density gradients directed toward the shocks. First-order Fermi acceleration upon reflection at each highly oblique shock front offsets loss by leakage through the shock front and sustains the particle intensity in the upstream region. Other acceleration mechanisms may not be required. A simple model is explored in which the gradient profile is primarily determined by a balance between shock sweeping and diffusive flow away from the shock (it is argued that acceleration by reflection and leakage through the shock cause a secondary modification of the profile). Profiles outside the compression region in 15 observations of corotating events suggest a radial mean free path lambda/sub r/=0.021..-->..0.64 AU (the mean is lambda/sub r/=0.23 AU) over r=2.6-6 AU. The model predicts an anisotropy which upstream of each shock is lower in magnitude than observations by a factor of approx. =2. The predicted direction in the upstream region is in the direction of corotation, i.e., perpendicular to the radius vector and counterclockwise in the ecliptic plane. Although net flows in this direction are observed, observations have not generally sought to distinguish upstream from downstream regions where net flows are expected to be approximately reversed.

• Research Organization: Oral Roberts University, Tulsa, Oklahoma 74171
• OSTI ID: 6931563
• Journal Information: J. Geophys. Res.; (United States), Journal Name: J. Geophys. Res.; (United States) Vol. 83:A5; ISSN JGREA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ACCELERATION
ANISOTROPY
BARYONS
ELEMENTARY PARTICLES
ENERGY RANGE
FERMIONS
HADRONS
MEAN FREE PATH
MEV RANGE
NUCLEONS
PLASMA ACCELERATION
PLASMA DENSITY
PROTONS
RADIATION STREAMING
RADIATIONS
SHOCK WAVES
SOLAR ACTIVITY
SOLAR PARTICLES
SOLAR PROTONS
SOLAR RADIATION
SOLAR WIND
STELLAR RADIATION