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Fig. 13


Radiation pressure efficiency (βrp) for grains around HD 15407 A as a function of grain size s for amorphous MgFeSiO4 (solid black), MgFeSi2O6 (red dashed), MgSiO3 (blue dotted), Mg2SiO4 grains (green dotted-dashed), crystalline Mg-rich and Fe-rich olivine grains (solid magenta, and dashed cyan) and β-cristobalite grains (dashed black). Shaded areas show regions where grains are gravitationally unbound to the star.

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