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Table 1

Initial conditions of the disc simulations.

Run M⋆,0 (M⊙) Rinit (AU) z Mdisc, 0 (M⊙) Ṁdisc (10−6M⊙yr−1)
01 0.2 60 1 0.040 1.80
02 0.2 60 0.1 0.040 1.80
03 0.2 60 10 0.040 1.80
04 0.2 90 1 0.050 2.25
05 0.2 90 0.1 0.050 2.25
06 0.2 90 10 0.050 2.25
07 0.2 120 1 0.059 2.63
08 0.2 120 0.1 0.059 2.63
09 0.2 120 10 0.059 2.63
10 0.3 60 1 0.049 2.70
11 0.3 60 0.1 0.049 2.70
12 0.3 60 10 0.049 2.70
13 0.3 90 1 0.062 3.38
14 0.3 90 0.1 0.062 3.38
15 0.3 90 10 0.062 3.38
16 0.3 120 1 0.072 3.95
17 0.3 120 0.1 0.072 3.95
18 0.3 120 10 0.072 3.95
19 0.4 60 1 0.057 3.60
20 0.4 60 0.1 0.057 3.60
21 0.4 60 10 0.057 3.60
22 0.4 90 1 0.071 4.50
23 0.4 90 0.1 0.071 4.50
24 0.4 90 10 0.071 4.50
25 0.4 120 1 0.083 5.26
26 0.4 120 0.1 0.083 5.26
27 0.4 120 10 0.083 5.26

Notes. The table lists: initial stellar mass (M⋆,0), disc radius (Rinit), metallicity (z), disc mass (Mdisc, 0), and mass loading rate (Ṁdisc). Disc masseswere set such that the Toomre parameter at the outer disc radius is Q = 10 (i.e. the discs areinitially gravitationally stable). The constant mass loading rate onto the disc was set from Eq. (5), where χ = 0.1. The disc metallicity was varied by modifying the opacities by a factor z.

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