Can gas in young debris disks be constrained by their radial brightness profiles?

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Table 1:

Models for ${\beta }$ Pic, HD 32297, and AU Mic.
	${\beta }$ Pic										HD 32297		AU Mic
Star
Luminosity, $L_\odot$	8.70										5.40		.092
Mass, $M_\odot$	1.75										1.80		.50
Age, Myr	12										30		12
Planetesimals and dust
Birth ring, AU	110-130										60-80		30-40
Max optical depth	$5 \times 10^{-3}$										$4 \times 10^{-3}$		$6 \times 10^{-4}$
Init. surf. density slope	-1.5										-1.5		-1.5
$[s_{\rm min}, s_{\rm max}]$ , $\mu\hbox{m}$	[1, 86]										[0.6, 52]		[0.04, 3.2]
Gas
Model identifier	000	tns	t0ns	t1ns	rns	r0ns	r1ns	ths	thf	tvs	tns	ths	tns	ths
t- or r-support	-	t	t	t	r	r	r	t	t	t	t	t	t	t
Temperature slope p	-	1/2	0	1	1/2	0	1	1/2	1/2	1/2	1/2	1/2	1/2	1/2
Mass, $M_\oplus$	-	.05	.05	.05	.05	.05	.05	5	5	50	.15	15	$2\times 10^{-4}$	$2\times 10^{-2}$
Surface density slope	-	-1.5	-1.5	-1.5	-1.5	-1.5	-1.5	-1.5	-1.0	-1.5	-1.5	-1.5	-1.5	-1.5
Outer edge, AU $^\star$	600										350		175

$^\star$ The arbitrary truncation distance (we set it to five times the central distance of the respective birth ring). It only affects the conversion of total gas mass to gas density. In that conversion, we also use a constant semi-opening angle of $15^\circ$ for all disks, assuming the density to be constant with height.

Source LaTeX | All tables | In the text

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