The Martian neutral winds, ion drifts, and ion fluxes are derived by reproducing the electron density profiles observed by the 
MAVEN/ROSE and Mars Express spacecraft. We use our 1-D chemical diffusive model to interpret the measured ionospheric structure 
at altitudes where plasma transport dominates. We find it is necessary to impose field-aligned vertical plasma drifts caused by 
the motion of neutral winds.  The following files can be used to reproduce the model results derived in this paper. Note that 
the units of the parameters are given in the header of each file. 


1) Best Fit_model_file_for_Figure2.dat. This file provides the best fitted electron density (Ne) (cm-3) profile to the Mars 
Express Ne (cm-3) profile. It aslo provides the corresponding ion densities. 
The header of this file reads as:  HEIGHT (cm) CO2+ (cm-3) CO+ (cm-3)  O2+ (cm-3)  O+ (cm-3)   NO+ (cm-3)  H+ (cm-3)   Ne (cm-3)


2) Best Fit_model_file_for_Figure3.dat. This file provides the best fitted electron density (Ne) (cm-3) profile to the 
MAVEN/ROSE Ne (cm-3) profile. It also provides the corresponding ion densities.
The header of this files reads as: HEIGHT (cm) CO2+ (cm-3) CO+ (cm-3)  O2+ (cm-3)  O+ (cm-3)   NO+ (cm-3)  H+ (cm-3)   Ne (cm-3)


3) Model_file_diffusive_equil_Figure2.dat. This file provides the model electron density (Ne) (cm-3) profile from simple 
model (with no top boundary ion fluxes and no vertical drift is applied) in comparison to the Mars Express Ne (cm-3) profile. 
The header of this files reads as:  Height (km)    Ne (cm-3)


4) Model_file_diffusive_equil_Figure3.dat. This file provides the model electron density (Ne) (cm-3) profile from simple 
model (with no top boundary ion fluxes and no vertical drift is applied) in comparison to the MAVEN/ROSE Ne profile.
The header of this files reads as: Height (km)    Ne (cm-3)


5) Model_file_for_flux_Figure4.dat.  This file provides the derived ion fluexes (cm-2 s-1) at the Mars Express location.
The header of this files reads as: Altitude (cm)  Co2+ (cm-2 s-1)   CO+ (cm-2 s-1)    O2+ (cm-2 s-1) 
 O+ (cm-2 s-1)     NO+ (cm-2 s-1)      H+ (cm-2 s-1) 


6) Model_file_for_flux_Figure5.dat.  This file provides the derived ion fluexes and vertical ion drifts (WD) at the 
MAVEN/ROSE location.
The header of this files reads as: Altitude (cm)  Co2+ (cm-2 s-1)   CO+ (cm-2 s-1)    O2+ (cm-2 s-1)                      
 O+ (cm-2 s-1)     NO+ (cm-2 s-1)      H+ (cm-2 s-1)


7) Model_WD_for_Figure4.dat.         This file provides the derived vertical ion drifts (WD) (cm/s) at the Mars Express location.
The header of this files reads as: Altitude(cm)  WD (cm/s)


8) Model_WD_for_Figure5.dat.         This file provides the derived vertical ion drifts (WD) (cm/s) at the MAVEN/ROSE location.
The header of this files reads as: Altitude(cm)  WD (cm/s)


Table2 shows the derived neutral wind speeds at MEX/MaRS and MAVEN/ROSE locations in the paper. The zonal (Un) and 
meridional (Vn) winds are the components in terms of Un sinδ and Vn cosδ.  Un and Vn are calculated from WD formulation 
given in the paper as equation 3. To reproduce this Table2, one needs to have the following parameters.


Ion-neutral collision frequency (νi) 
Ion Gyro-frequency (Ωi)
Magnetic inclination angle (I)
Magnetic declination angle (δ)


These parameters are given in files MEX-MaRS_Table2.dat and MAVEN-ROSE_Table2.dat at different altitudes (in km) at MEX/RaRS and 
MAVEN-ROSE locations, respectively.


The header of MEX-MaRS_Table2.dat file reads as: Altitude (km)    νi (1/s)    Ωi (1/s)    I (deg)   δ (deg)
The header of MAVEN-ROSE_Table2.dat file reads as: Altitude (km)    νi (1/s)    Ωi (1/s)    I (deg)   δ (deg)