Numerical modeling of impact survival and atmospheric escape shows Mars ejecta smaller than 0.03 m rarely deliver viable microbes to Phobos orbit due to drag and heating.
Time history of aerodynamic heat transfer rate at the forebody stagnation point is determined by Tauber’s formula (Tauber et al., 1990; Tauber and Sutton
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Assessment of the probability of microbial contamination for sample return from Martian moons I: Departure of microbes from Martian surface
Numerical modeling of impact survival and atmospheric escape shows Mars ejecta smaller than 0.03 m rarely deliver viable microbes to Phobos orbit due to drag and heating.