Model of the Earth's Bow Shock

	Results by:		Lee Bennett
	From the paper:		A Model of the Earth's Distant Bow Shock   by L. Bennett, M. G. Kivelson, K. K. Khurana, L. A. Frank, W. R. Paterson (to be published in the Journal of Geophysical Research, 1997.)

readme   Contains a brief explanation of the methods used and a description of each program file.

Source Code

x_rho.f

x_rho.f will take arbitrary solar wind conditions as input and give an x - rho profile of the bow shock for those conditions.

y_z.f

y_z.f will take arbitrary solar wind conditions as input and give a y - z profile of the bow shock for those conditions.

Paper

Text

Postscript file of the text of out paper to be published in the Journal of Geophysical Research, 1997.

Figure 1

Postscript file of figure 1 in the paper. Data for the portions of Galileo's second flyby of Earth containing clear shock encounters. The unshaded regions of the graph are times when the spacecraft was in the solar wind. The lighter shaded regions are times when Galileo was in the magnetosheath. The darkest shaded regions are periods when disturbed solar wind conditions made the accurate identification of shocks difficult.

Figure 2

Postscript file of figure 2 in the paper. Positions of Galileo shock encounters compared with the F/G model. The dots are the position of Galileo in a cylindrical, aberrated GSE coordinate system at each shock crossing. The solid line is the F/G model.

Figure 3

Postscript file of figure 3 in the paper. Construction of the asymptotic bow shock adapted from Spreiter et al [Planet. Space Sci., 14, 223, 1996.]

Figure 4

Postscript file of figure 4 in the paper. Illustration of how the KK94 method is used to modify the base model.

Figure 5

Postscript file of figure 5 in the paper. Comparisons between the measured shock locations and models modified using the KK94 method. The circles are the observations from December 5, 1992 and the dotted line is our model for that day. The triangles and the dashed line are for the period from late December 6 to early December 7. The squares and the dot-dashed line are for late December 7. The solid line is the F/G model.

Figure 6

Postscript file of figure 6 in the paper. Difference between the cylindrical radius at Galileo's position and the model for December 5, 1992. The location of the shock encounters re identified from jumps in the total magnetic field and shading shows when the spacecraft was in the magnetosheath.

Figure 7

Postscript file of figure 7 in the paper. Model of the bow shock at the time of Galileo's first flyby of Earth on December 5, 1990.

Figure 8

Postscript file of figure 8 in the paper. Shock crossings observed by Pioneer 7 during September 1966 Villante [JGR, 81, 1441, 1976] compared with the predictions of our models for conditions at the time of each crossing.

Figure 9

Postscript file of figure 9 in the paper. Magnetic field and velocity data from December 5, 1992 plotted in a shock normal coordinate system. The shock normal was calculated using the model of the shock on December 5, 1992 obtained using the KK94 method. The shock crossings are identified using the total magnetic field and density and shading shows when the spacecraft was in the magnetosheath.

Figure 10

Postscript file of figure 10 in the paper. Density compression ratio and magnetic compression observed by Galileo (solid circles) on December 5, 1992 and calculated (open circles) by solving the Rankine Hugoniot equations using a shock normal from the model. The data are plotted versus downtail distance.

Figure 11

Postscript file of figure 11 in the paper. Cuts through the model bow shock showing changes when one solar wind parameter is varied keeping the others constant.

Figure 12

Postscript file of figure 12 in the paper. Series of models using the Farris and Russell [JGR, 99, 17681, 1994] theory of the sunward motion of the bow shock for low Mach numbers.

Figure 13

Postscript file of figure 13 in the paper. Series of models using the Farris and Russell [JGR, 99, 17681, 1994] theory of the sunward motion of the bow shock for low Mach numbers.using the Cairns and Lyon [JGR, 100, 17173, 1995] theory of the sunward motion of the bow shock for low Mach numbers.

Figure 14

Postscript file of figure 14 in the paper. Comparisons between the measured shock locations and models modified using the epsilon adjustment method.

 

Last Updated: April 10, 1998