Modeling Ion Transport in the Upper Ionosphere of Mars: Exploring the Effect of Crustal Magnetic Fields (Dataset)

Abstract

The data in this repository was produced via the model presented in the paper referenced in this readme file. Each folder contains data from a different case presented in the paper. Case 1 is a low altitude closed crustal magnetic field line, Case 2 is a high altitude closed crustal magnetic field line, Case 3 is a high altitude open crustal magnetic field line, and the Non-Crustal case is a case with no influence from the crustal magnetic fields.

For Cases 1, 2, and 3, each folder contains subfolders labeled run1 through run9. Each run is 10,000 seconds of modeled time. The total time for each case is 90,000 seconds, which is slightly longer than one Mars day, so one full day is modeled. Each case starts with time=0 with Mars rotated to 83° past local noon. run1 goes from angle of rotation (with respect to local noon) of 83.08° to 123.69° (late dayside/dusk/early nightside). run2 goes from angle of rotation of 123.69° to 164.30° (early nightside). run3 goes from angle of rotation of 164.30° to 204.91° (nightside through midnight). run4 goes from angle of rotation of 204.91° to 245.52° (late nightside). run5 goes from angle of rotation of 245.52° to 286.14° (late nightside/dawn). run6 goes from angle of rotation of 286.14° to 326.75° (early dayside). run7 goes from angle of rotation of 326.75° to 7.36° (dayside through noon). run8 goes from angle of rotation of 7.36° to 47.97° (mid/late dayside). run8 goes from angle of rotation of 47.97° to 88.58° (late dayside).

In each run# subfolder, there are density and velocity files for each ion species, as well as an electron density file. (ex: o2+_densities.txt)

The first line of each density file has a heading to label the respective species, variable (density), and units (1/m^3). The second line of each file acts as column headers for each column. The remaining lines are model grid points. The first column is index: i; the second column is distance along the field line (units in meters): s[m]; the third column is altitude (units in kilometers): alt[km]; the fourth column is density (units in 1/m^3) for the initial time point of that run: t=XX. Each remaining column is density (units in 1/m^3) at the time point (units in seconds) of the column header. ex: say column #7 is headed by 3000.00. The values listed in this column are the density results at time = 3000.00 seconds.

The first line of each velocity file has a heading to label the respective species, variable (velocity), and units (m/s). The second line of each file acts as column headers for each column. The remaining lines are model grid points. The first column is index: i; the second column is distance along the field line (units in meters): s[m]; the third column is altitude (units in kilometers): alt[km]; the fourth column is velocity (units in m/s) for the initial time point of that run: t=XX. Each remaining column is the velocity (units in m/s) at the time point (units in seconds) of the column header. ex: say column #7 is headed by 3000.00. The values listed in this column are the velocity results at time = 3000.00 seconds.

For the Non-Crustal case, the folder contains one file: densityprofiles_noncrustal.txt. This file contains density results for the non crustal case. The first line of the file acts as column headers. The remaining lines are model grid points. The first column is index: i; the second column is altitude (units in kilometers): Alt. The remaining headers denote the species.