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Using warm dust to constrain unseen planets

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Figure

Figure 1. A schematic diagram of our approach, indicating thethe planet, going on to hit the star (accreted by the planet (the fraction of particles ejected by the planet (location of the initial belt in the N-body simulations which trackFej), the fractionFacc) and the fraction that migrate pastFpast), as described in §2.
Figure 2. The results of the numerical simulations showing thefraction of particles ejected as a function of planet mass, for β =0.1 (top panel), planet semi-major axis, for β = 0.1 (middle panel)and particle size, for apl = 1au (β Eq
Figure 3. The results of the numerical simulations showing the
Table 1. The analytic and numerical values of the constants inpredicting the fraction of particles ejected of the form Eq
+7

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