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Table 10

Magnitude brightening distribution as a function of heliocentric distance organized by Oort group.

Brightening in magnitudes from r to 1 au
Oort group r (au) μ σ 10% 25% 50% 75% 90% N
New 1 0.00 0.00 0.00 0.00 0.00 0.00 0.00 13
2 1.82 1.48 0.24 0.67 1.68 2.45 3.26 12
3 3.79 2.09 1.53 2.38 3.70 5.22 5.85 11
4 5.27 2.42 2.81 3.20 5.32 7.00 8.54 10
5 6.70 2.68 3.53 4.80 6.40 8.95 9.90 8
6 6.58 1.92 4.68 5.26 6.73 6.80 8.35 6
7 6.33 1.47 5.12 5.14 6.07 7.26 7.77 4
8 8.02 1.28 6.79 7.38 8.13 8.77 9.15 4
9 9.30 1.41 8.50 8.80 9.30 9.80 10.10 2

Intermediate 1 0.00 0.00 0.00 0.00 0.00 0.00 0.00 16
2 3.12 1.57 1.36 1.66 3.25 4.51 5.07 14
3 4.56 1.54 2.62 3.64 4.85 5.33 5.40 12
4 5.77 1.77 3.80 4.47 5.80 6.80 7.65 11
5 6.85 1.95 4.76 6.41 7.60 8.10 8.34 5
6 8.16 2.47 5.77 7.50 8.20 9.10 10.49 5
7 8.00 2.61 6.52 7.07 8.00 8.92 9.48 2
8 8.97 1.94 7.36 8.16 9.50 10.05 10.38 3
9 9.36 2.32 8.05 8.54 9.36 10.18 10.67 2

Old 1 0.00 0.00 0.00 0.00 0.00 0.00 0.00 15
2 3.17 1.95 0.80 1.32 3.90 4.50 4.68 13
3 5.37 2.44 2.86 3.89 5.25 6.33 8.70 10
4 7.63 4.17 4.03 4.30 6.22 10.18 12.23 5
5 8.84 4.91 5.82 6.00 6.31 10.40 12.86 3
6 2.70 4.53 10.14 11.10 12.70 14.30 15.26 2

Notes. Each row lists average and standard deviation, plus quantiles (based on sample of size N) of how many magnitudes a comet will brighten from a given heliocentric distance to 1 au. See text for details.

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