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Martian bow shocks, the solar wind interacting with an unmagnetized planet,are studied. We theoretically investigated how solar parameters, such as thesolar wind dynamic pressure and the solar extreme ultraviolet (EUV) flux,influence the bow shock location, which is still currently not well understood.We present the formula for the location of the bow shock nose of theunmagnetized planet. The bow shock location, the sum of the ionopause locationand bow shock standoff distance, is calculated in the gasdynamics approach. Theionopause location is determined using thermal pressure continuity, i.e., thesolar wind thermal pressure equal to the ionospheric pressure, according totangential discontinuity. The analytical formula of the ionopause nose locationand the ionopause profile around the nose are obtained. The standoff distanceis calculated using the empirical model. Our derived formula shows that theshock nose location is a function of the scale height of ionosphere, thedynamic pressure of the solar wind and the peak ionospheric pressure. Thetheoretical model implies that the shock nose location is more sensitive to thesolar EUV flux than solar wind dynamics pressure. Further, we theoreticallyshow that the bow shock location is proportional to the solar wind dynamicpressure to the power of negative C, where C is about the ratio of theionospheric scale height to the distance between bow shock nose and the planetcenter. This theory matches the gasdynamics simulation and is consistent withthe spacecraft measurement result by Mars Express [Hall, et al. (2016) J.Geophys. Res. Space Physics, 121, 11,474-11,494].

Theoretical investigation of the bow shock location for the solar wind interacting with the unmagnetized planet