Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21a0484w&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #SH21A-0484
Physics
2134 Interplanetary Magnetic Fields, 2152 Pickup Ions, 7843 Numerical Simulation Studies
Scientific paper
We use a multi-fluid, spherically symmetric, MHD model with neutral hydrogen and pickup protons, with 1999 solar wind data at 1 AU as input, to calculate the magnetic field strength (B) profiles that would be observed at various points between 1 and 60 AU with a resolution of 1 day over an interval of ¯ 1 year. The model predicts the following statistical results for daily averages of B: 1) the distribution functions of B are approximately lognormal at all distances from 1 to 60 AU; 2) the standard deviation of B divided by the mean value of B, $, for a magnetic field profile at a given distance is approximately a constant, independent of distance between 10 and 60 AU; and 3) the power spectrum of B/$ evolves such that a) at small scales the power spectral density decreases with increasing distance from the Sun, b) at large scales the power spectral density increases with distance, and c) there is a range of frequencies in which the power spectrum is a power law, the power law extending to lower frequencies with increasing distance. All three of these results have been observed by the Voyager 1 and 2 spacecraft over the last 20 years, between 1 and ¯ 60 AU. The agreement between the observations made over many years and the results of the model with input from 1 AU during 1999 suggests that the statistical state of the heliosphere is not very sensitive to the initial conditions.
Burlaga Leonard Francis
Richardson John D.
Wang Chenjie
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