Observations of 35- 10 1600-keV protons and low-frequency waves upstream of interplanetary shocks

Details Observations of 35- 10 1600-keV protons and low-frequency waves upstream of interplanetary shocks Observations of 35- 10 1600-keV protons and low-frequency waves upstream of interplanetary shocks

May 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985jgr....90.3973s&link_type=abstract

(American Geophysical Union, Chapman Conference on Collisionless Shock Waves in the Heliosphere, Napa Valley, CA, Feb. 20-24, 19

Physics

36

Interplanetary Magnetic Fields, Low Frequencies, Polarization (Waves), Shock Wave Interaction, Solar Protons, Bow Waves, Doppler Effect, Flux Density, International Sun Earth Explorer 3, Power Spectra, Proton Energy, Solar Flares

Scientific paper

The present investigation is concerned with a comparison of measurements of energetic protons in the range from 35 to 1600 keV and low-frequency waves (periods of approximately 6 s) on ISEE 3 associated with the passage of the large oblique shock of April 5, 1979, which exhibits an extended foreshock. An attempt is made to identify the energy of the particles which are responsible for the waves. Intensity profiles of both waves and particles as a function of upstream distance are compared, taking into account the relation between the energy of the particles and the period of the waves. The considered approach makes it possible to identify protons with energies of a few hundred keV as being responsible for the waves in the extended foreshock. It is believed that the high energy density of the high-energy solar flare protons preceding the shock could be responsible for 'seed' waves which provide the scattering centers necessary for the acceleration of the lower-energy protons via a first-order Fermi mechanism.

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