The dust coma environment of the short period comets 32P/Comas Solá, 56P/Slaughter-Burnham, and 78P/Gehrels 2 from ground-based observations

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Table 8

Summary of grain velocity obtained from the application of the inverse numerical model, for several comets at the heliocentric distances where our target comets have been observed.

Comet	Ref.	Reference grain size	Heliocentric distance^a	Grain velocity^b
		[cm]	[AU]	[m/s]

6P/d’Arrest	(1)	0.1	2.02	10
			2.44	...
			2.65	...
46P/Wirtanen	(2)	0.01	2.02	23
			2.44	15
			2.65	13
65P/Gunn	(2)	0.01	2.02	...
			2.44	...
			2.65	24
67P/Churyumov-Gerasimenko	(3)	1	2.02	9^I, 2°
			2.44	...
			2.65	...
103P/Hartley 2	(4)	0.1	2.02	4
			2.44	3
			2.65	3

References. (1): Fulle (1990); (2) Colangeli et al. (1998); (3) Fulle et al. (2004); (4) Epifani et al. (2001).

Notes.

^(a)

r = 2.02 AU refers to our 78P/Gehrels 2 observation. r = 2.44 AU refers to our 32P/Comas Solá observation. r = 2.65 AU refers to our 56P/Slaughter-Burnham observation.

^(b)

I refers to preperihelion, O to postperihelion.

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