Forming Earth-like and low-mass rocky exoplanets through pebble and planetesimal accretion

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Table 2

Simulation parameters for different stars.

Parameter	1.00 M_⊙	0.70 M_⊙	0.49 M_⊙	0.20 M_⊙	0.09 M_⊙
Initial disc mass (M_D,0) (M_⊙)	0.050	0.035	0.025	0.010	0.009
Initial planetesimal ring mass (M_pl,0) (M_E)	0.015	0.015	0.015	0.015	0.010
Wide planetesimal ring size (r_pl,min,w–r_pl,max,w) (au)	0.2–2.2	0.2–2.0	0.2–1.0	0.2–0.8	0.2–0.8
Narrow planetesimal ring size (r_pl,min,n–r_pl,max,n) (au)	1.18–1.60	0.92–1.25	0.72–0.97	0.38–0.52	0.30–0.40
Disc inner radius (r_in) (au)	0.097	0.086	0.076	0.057	0.021
Inner truncation radius (r_trunc) (au)	0.046	0.041	0.037	0.027	0.013
Total pebble mass flux ( $\int {\dot{M}}_{F} d t$ $\[\int \dot{M}_{\mathrm{F}} \mathrm{d} t\]$ ) (M_E)	217.0	118.7	65.0	14.3	7.4

Notes. The total pebble mass flux is not an input parameter, but is calculated by integrating Eqs. (7) and (10).

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