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Table 3

Description of ACE runs.

Disc type Extenta r-distr.b Ṁ ⋆ c e max d i max e Materialf M d g h M min i Grid resol.j Sect.k
[au] [Ṁ⊙] [rad] [ M⊕ ] [m] [ M⊕ ]
Narrow outer PB 37.5−42.5 ∝ r0 0 0.03 0.015 M1 1.5 × 10-3 20 0.02 m1,e1,p1 4.1
50 1.7 × 10-3 100 0.05
300 2.1 × 10-3 250 0.1
37.5−42.5 ∝ r0 50 0.03 0.015 M2 2.4 × 10-3 100 0.06 m1,e1,p1 4.2
M3 1.5 × 10-3 100 0.05
M4 1.4 × 10-3 200 0.05
37.5−42.5 ∝ r0 50 0.01 0.005 M1 1.7 × 10-3 30 0.05 m1,e1,p1 4.3
0.1 0.05 6.4 × 10-4 100 0.03
Extended outer PB 25.5−42.5 ∝ r0 50 0.03 0.015 M1 1.7 × 10-3 100 0.08 m1,e1,p1 4.4
1.0−45 ∝ r-1.5 2.1 × 10-3 100 0.2 m2,e1,p1
Narrow inner PB 2.8−3.2 ∝ r0 50 0.03 0.015 M1 6.2 × 10-6 1 × 105 0.02 m1,e1,p2 5
M3 5.4 × 10-6 4 × 105 0.02
M5 4.5 × 10-6 4 × 105 0.02

Notes.

(a)

Radial extent of the planetesimal belt;

(b)

specification of the radial distribution of planetesimals;

(c)

stellar mass loss rate in units of the solar value;

(d)

maximum eccentricity of the planetesimal orbits;

(e)

semi-opening angle of the planetesimal disc;

(f)

name of dust material used (symbol explanation in Table 2);

(g)

derived dust mass (grains up to 1 mm in radius);

(h)

object size for which the collisional lifetime equals the physical age of the AU Mic system;

(i)

estimated minimum total disc mass (grains up to size );

(j)

specification of grid: 37 bins in mass from 5 × 10-18 to 1 × 1010 g (m1), 40 bins in mass from 8 × 10-18 to 1 × 1013 g (m2), 22 bins in eccentricity from 0.001 to 2 (e2), 30 bins in pericentric distance from 1 to 60 au (p1), 20 bins in pericentric distance from 0.1 to 7 au (p2);

(k)

section number in this work where the runs are addressed.

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