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tokens: Samsonov et al. (2020) that r 0 would be predicted more accurately by taking the effects of ρ SW and V SW individually into account rather than considering P d alone. However, Samsonov et al. (2020) also indicated that the changes in r 0 for a velocity change were greater than those for a density change for the same P d , especially for a southward IMF, which implied that the power-law index of V SW , M , was lower than that of ρ SW , N . We found a different result, however: A higher solar wind number density (or a lower velocity) results in a smaller r 0 of the Martian MPB for thesame P d ( M > N ). Moreover, these two results are also inconsistent with the results of Ramstad et al. (2017) , who reported that the Martian IMB was mainly pressure-dependent and that changing ρ SW or V SW individually had no significant effect for the equal dynamic pressure. The mechanism for the different effects of ρ SW and V SW on r 0 for the Earth can be explained by the solar wind electric field. It is generally greater for a higher solar wind velocity, which leads to the enhanced magnetopause reconnection rate and Region 1 current, especially for a southward IMF (e.g., Lee Lee 2020 ; Samsonov et al. 2020 ). As a result, the greater changes in r 0 occur for a velocity increase and not for a density increase for the same P d . For Mars, which is a weakly magnetized planet, the different results of ρ SW and V SW effects cannot be explained by the traditional concept of the solar wind electric field and the reconnection conditions at the Earth. On the other hand, the location of the magnetopause can also be affected and described by the pressure balance across it, as we mentioned above. To investigate the reason for the opposite effects of ρ SW and V SW at Mars as compared to Earth, we next studied the pressure balance throughout the MPB in more detail. Following Schield (1969) and Suvorova et al. (2010) , we introduced a factor k and f that describe the contributions of the different components, both thermal and magnetic, of pressure to the total pressure. We define the factor k as the ratio of the total pressure just outside the Martian MPB to the upstream solar wind dynamic pressure as follows: . Here , , and are the plasma thermal pressure, the magnetic pressure, and the solar wind dynamic pressure just outside the subsolar standoff point of the Martian MPB, respectively. is the solar wind dynamic pressure upstream of the bow shock. As the plasma thermal pressure and the magnetic pressure upstream of the bow shock are very low and can be neglected, the factor k can be used to describe how much the upstream solar wind dynamic pressure is converted into thermal and magnetic pressure just outside the MPB. The theoretical value of k in a gas-dynamic approximation assuming a normal shock is 0.881 ( Schield 1969 ). In addition, k also varies with the upstream solar wind and downstream magnetopause conditions (e.g., Suvorova et al. 2010 ). For a higher value of