Can dust coagulation trigger streaming instability?

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Table 1

Overview of parameters used and results obtained in different runs.

Run name	Π^a	Z_tot^b	v_f^c	M_plts/M_tot^d	t_plts^e

P2Z7V5000			5000	83%	60
P2Z7V1000	0.02	0.07	1000	80%	64
P2Z7V100			100	78%	174

P2Z5V5000			5000	77%	85
P2Z5V1000	0.02	0.05	1000	73%	88
P2Z5V100			100	68%	212

P2Z3V5000			5000	61%	147
P2Z3V1000	0.02	0.03	1000	54%	151
P2Z3V100			100	47%	275

P5Z7V5000			5000	64%	59
P5Z7V1000	0.05	0.07	1000	57%	63
P5Z7V100			100	43%	175

P5Z5V5000			5000	50%	83
P5Z5V1000	0.05	0.05	1000	40%	88
P5Z5V100			100	20%	227

P5Z3V5000			5000	16%	233
P5Z3V1000	0.05	0.03	1000	0.8%	693
P5Z3V100			100	0%	–

P8Z7V5000			5000	35%	56
P8Z7V1000	0.08	0.07	1000	32%	61
P8Z7V100			100	0%	–

P8Z5V5000			5000	9%	125
P8Z5V1000	0.08	0.05	1000	5%	201
P8Z5V100			100	0%	–

Notes. Columns (a)−(c): parameters used in each run, Cols. (d), (e): results obtained;

^(a)

radial pressure gradient measure (Eq. (10));

^(b)

total vertically integrated dust-to-gas ratio;

^(c)

fragmentation velocity in cm s^-1;

^(d)

total final mass of planetesimals produced with respect to the initial total mass of dust;

^(e)

time when the planetesimal formation started in local orbital timescales.

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