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tokens: of orders of magnitude (Dong et al. 2018b ), thereby potentially attaining values as high as ∼0.1 mJy for weak magnetic fields. 3.2. Atmospheric Escape Next, we direct our attention to the central issue of atmospheric ion escape facilitated by the stellar wind in conjunction with the stellar radiation. Figure 2 depicts the pressure balance arising from the stellar wind–planet interactions. The first and second columns present the unmagnetized Venus-like and magnetized Earth-like cases, respectively. As a result of the supermagnetosonic nature of the stellar wind at TOI-700 d, bow shocks are formed ahead of this planet, regardless of the inclusion of the planetary magnetic field. Compared to the unmagnetized Venus analog, the presence of the global magnetic field results in a larger interaction cross-section with the stellar wind for the magnetized Earth-like case. An inspection of the bottom panels of Figure 2 reveals that the planetary magnetosphere (or induced magnetosphere for unmagnetized cases) is compressed, and the total pressure becomes intensified due to the stronger stellar wind pressure. Figure 2. Logarithmic scale contour plots of the total pressure ( P total , units of nPa)—the sum of the ion ( P ion ) and electron ( P electron ) pressure—in the meridional plane based on the stellar wind conditions at P min (first row) and P max (second row). The first column shows the unmagnetized Venus-like case, while the second column depicts the magnetized Earth-like case. The salient results concerning atmospheric escape are depicted in Figure 3 , which shows the calculated oxygen ion density with the associated magnetic field lines in the meridional plane for all six cases. This figure yields some general conclusions. To begin with, as seen from Table 1 , we note that O + constitutes the dominant ion species undergoing escape for all configurations considered here. The atmospheric oxygen escape rates vary from s −1 to s −1 , indicating that they are higher by a few orders of magnitude than the typical escape rates of ) s −1 for the terrestrial planets in our solar system (e.g., Dong et al. 2017b , 2018c ). Figure 3. Logarithmic scale contour plots of the O + ion density (units of cm −3 ) with magnetic field lines (in white) in the meridional plane based on the stellar wind conditions at P min (first row) and P max (second row). The first column shows the unmagnetized Venus-like cases, whereas the second and third columns depict the unmagnetized and magnetized Earth-like cases. Let us first compare the unmagnetized cases, namely, the first and second columns. We find that the Earth-like case exhibits a stronger and broader flux of escaping O + compared to the Venus-like case; this result is also consistent with the atmospheric ion escape rates shown in Table 1 . The reason chiefly stems from the fact that the upper atmosphere of a Venus analog is cooler than its Earth-like counterpart due to the efficient CO 2 cooling caused by 15 μ m