Terrestrial Accretion from the Solar Wind

Details Terrestrial Accretion from the Solar Wind Terrestrial Accretion from the Solar Wind

Apr 1961

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1961natur.190..156d&link_type=abstract

Nature, Volume 190, Issue 4771, pp. 156 (1961).

Physics

9

Scientific paper

IN order to account for the observed motions of comet tails, Biermann1 conceived that the solar corona emits suprathermal particles at the rate of 1014-1015 gm./sec. Since this material is evidently supplied by the Sun itself, this seems to imply that Unno's observation2 of turbulent motions in the chromosphere and lower corona corresponds in reality to a systematic radial emission of particles from the Sun, the velocity v of which is related to the hydrogen ion concentration n by the relation v = Bn-1/4, where B = 8 × 108 (cm.)1/4 sec.-1. This empirical relation is of the same form as Parker's magneto-hydrodynamical velocity-amplitude relation3,4, v(r) = v0(no/nr)1/4, the applicability of which is certainly not restricted to the chromosphere. Thus the possibility of extrapolating Unno's result to interplanetary space deserves further consideration.

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