Planet formation around M dwarfs via disc instability - Fragmentation conditions and protoplanet properties

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Table 2

Results for the disc simulations with the initial conditions listed in Table 1 after 30 kyr of evolution.

Run	M_⋆ (M_⊙)	M_disc (M_⊙)	ΔM_disc (M_j)	t (kyr)	q	R_disc (AU)	a_frag (AU)
01	0.205	0.075	36.6	22.1	0.37	75	49
02	0.205	0.077	38.9	23.3	0.38	72	35
03	–	–	–	–	–	–	–

04	0.205	0.104	56.2	25.9	0.51	92	54
05	0.206	0.105	57.2	27.6	0.51	137	55
06	0.207	0.106	58.1	28.0	0.51	169	32

07	0.204	0.124	68.7	26.7	0.61	144	46
08	0.205	0.126	70.8	27.6	0.62	128	30
09	0.207	0.128	72.2	28.8	0.62	190	54

10	0.305	0.094	46.9	18.5	0.31	96	40
11	0.305	0.097	50.2	19.6	0.32	68	32
12	–	–	–	–	–	–	–

13	0.305	0.122	63.0	19.2	0.40	89	59
14	0.305	0.125	66.3	20.2	0.41	89	28
15	–	–	–	–	–	–	–

16	0.304	0.146	77.8	20.0	0.48	131	55
17	0.305	0.150	81.7	21.0	0.49	126	60
18	0.307	0.155	86.7	22.7	0.50	159	84

19	–	–	–	–	–	–	–
20	–	–	–	–	–	–	–
21	–	–	–	–	–	–	–

22	0.405	0.144	76.2	17.3	0.36	105	57
23	0.405	0.140	72.1	16.4	0.35	91	37
24	–	–	–	–	–	–	–

25	0.405	0.165	86.1	16.5	0.41	123	47
26	0.405	0.171	91.6	17.6	0.42	130	43
27	0.407	0.176	97.4	19.0	0.43	164	116

Notes. M_⋆ and M_disc are respectively the masses of the star and disc when the disc fragments. t is the time at which fragmentation occurs, q is the disc-to-star mass ratio at fragmentation and R_disc is the radius of the disc. a_frag is the distance of the fragment from the host star. Some discs did not fragment as noted by dashes in the corresponding rows.

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