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Fig. 11

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Collision probability with Mars (using its current orbital and physical properties) per orbital revolution as a function of the projectile perihelion distance (qp) divided by Mars’ perihelion distance (qt) according to the Hill sphere method. The probability peaks when this ratio equals unity, and the variation is the same for both dynamical models used: the two-body problem (2BP) and the restricted 3-body problem (R3BP).

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