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

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Table 2

Characteristics of the episodic accretion events.

Model	#	τ_eae [Myr]	R_gap (τ_eae) [AU]	f_eae
no X-ray	660	1.90	−	−
L_X = 10²⁹	315	0.99	−	−
L_X = 10³⁰	101	0.34	11.8	0.002
L_X = 10³¹	55	0.18	32.7	0.03
low_alpha	68	0.32	28.6	0.03
low_Bstar	46	0.17	29.0	0.05

Notes. The hash symbol (#) denotes the number of episodic accretion events. The unit of the X-ray luminosities is erg per second (erg s⁻¹).

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