Energetic electrons of terrestrial origin behind the bow shock and upstream in the solar wind
Summary (1 min read)
- Out to be isotropic, the hypothesis (An('erson, 1968) that fast-ii ► odc waver, propagating upstream from the shock cotiple to the solar wind to accelerate particles would be favored.
- A remarkable feature of the bow shock spikes is that they have large intensity just behind the bow shock and rapidly decreasing intensity moving either toward or away from the magnetosphere .
- This close confinement means that a relatively small total number of energetic particles can produce an appreciable flux without excessive demands on the source strength which presumably acts only in a sinall region behind the shock.
- This idea was used by Jokipii and Davis (1964) in their theoretical analysis of the bow shock spikes.
- Just what the magnetic field configuration is that produces a mirror geometry is less clear.
- Ileppner, et al. (1967) have shown that at the shock the field strength rises by several gammas above the average magnetosheath field.
- Evieleritly this only way to avoid the conclusion that the p; ► i•ticIvs are confined is to postulate a reversible effect by which particles ary accelerated behind the shock but when they leave this region they become deceleratcd.
- They have a strong tendency to appear oil dawn :Hide as expected from the average; spiral character of the inLerplanetary magnetic field .
- This kind of measurement could in principle, be made with two spacecraft.
- They ranged from 2 to 6 minutes but a great deal of spectral power was also spread over longer periods.
- The situation concerning bow shock spikes now appears to be that they represent an interesting case of particle acceleration by solar wind interaction with the earth's magnetosphere.
Did you find this useful? Give us your feedback
Related Papers (5)
J. R. Asbridge, S. J. Bame +1 more
B. U. Ö. Sonnerup
C. S. Wu
R. P. Lin, C. I. Meng +1 more
M. M. Leroy, A. Mangeney