Probabilistic models of the Jovian magnetopause and bow shock locations

Details Probabilistic models of the Jovian magnetopause and bow shock locations Probabilistic models of the Jovian magnetopause and bow shock locations

Oct 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jgra..107.1309j&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 107, Issue A10, pp. SMP 17-1, CiteID 1309, DOI 10.1029/2001JA009146

Physics

Plasma Physics

24

Magnetospheric Physics: Magnetopause, Cusp, And Boundary Layers, Interplanetary Physics: Planetary Bow Shocks, Space Plasma Physics: Numerical Simulation Studies, Planetology: Solar System Objects: Jupiter, Planetology: Fluid Planets: Magnetospheres (2756)

Scientific paper

New three-dimensional models of the Jovian magnetopause and bow shock were derived by combining spacecraft observations with boundary characteristics inferred from a magnetohydrodynamic (MHD) simulation. The MHD simulation provides polynomial forms parameterized by solar wind dynamic pressure. Observations from Pioneer 10 and 11, Voyager 1 and 2, Ulysses, and Galileo were used to establish the probability that regions surrounding Jupiter fall inside or outside these boundary surfaces. The magnetopause location was found to have a bimodal probability distribution with the two most probable standoff distances at 63 RJ (σ = 4 RJ) and 92 RJ (σ = 6 RJ). The bow shock location distribution appears bimodal, but a single distribution function description cannot be ruled out at the 95% confidence level. The mean bow shock standoff distance is 84 RJ (σ = 16 RJ). Analysis of solar wind measurements near 5.2 AU (interplanetary magnetic field, dynamic pressure, and Alfvén Mach number) suggests that the bimodal distribution of boundary positions results at least in part from the bimodal distribution of solar wind parameters in the vicinity of Jupiter. The probability density distributions of these parameters within and between regions of disturbed solar wind, caused by corotating interaction regions and coronal mass ejections, are statistically distinct. Smaller variations were also observed in these parameters over the solar cycle.

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