Time-dependent, long-term hydrodynamic simulations of the inner protoplanetary disk - III. The influence of photoevaporation

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Fig. 3

Disk evolution for different X-ray luminosities. The blue, black, red, and yellow lines correspond to an X-ray luminosity of L_X = 10³¹, 10³⁰, 10²⁹ ergs⁻¹, and no X-ray luminosity, respectively. Panel a, b, and c show the mass accretion rate on the star, ${\dot{M}}_{⋆}$ $\[\dot{M}_{\star}\]$ ; the width of the photoevaporative gap, R_gap; and the outer edge of the dead zone, R_DZ, respectively.

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