Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1971
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1971ap%26ss..10..471g&link_type=abstract
Astrophysics and Space Science, Volume 10, Issue 3, pp.471-485
Astronomy and Astrophysics
Astrophysics
10
Scientific paper
A complete solution has been obtained of the steady-state transport equations, including energy losses, for cosmic-rays in the interplanetary region for conditions in which diffusive transport is negligible and convective effects dominate. The region of validity of the solution will in general be a shell between heliocentric radiiR 1 andR 2 (R 2 may be infinite). The precise range of kinetic energyT and heliocentric radiusr in which the solution is valid is not known but it appears to be applicable in the vicinity of Earth to protons withT≤1 MeV. ForT˜0.5 MeV near Earth,R 1 may be ˜0.5 AU andR 1 will decrease asT, observed near Earth, decreases. The solution is simple in form but quite general; it predicts the differential number densityU (r, T) in terms of that observed at radius a (near Earth, say). Thus it may be quite useful in interpreting and co-ordinating steady-state cosmicray observations atT˜1 MeV. The differential and integral intensities, differential anisotropy and differential radial-gradient at (r, T) also are determined. A simple interpretation of the solution is given in terms of energy losses due to adiabatic deceleration of the particles as they are being convected outward from the Sun. This leads to the useful notion of following a particle in (r, T) as it increasesr and decreasesT. Particles convected from the outer corona to Earth decrease their kinetic energy by factor ˜500.Following a particle the Compton-Getting factor remains constant. Particles observed at (a, T) in convective transport have come from nearer the Sun; they may be of solar origin but may also be of galactic origin having penetrated tor
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