On the interplay between flaring and shadowing in disks around Herbig Ae/Be stars

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Table 1:

Model parameter ranges.
Parameter	Values
$\log ~ m$ [ $M_\odot$ ]	-3, -4, -5, -6, -7
p	1, 1.5, 2
i	10 $^\circ$ -90 $^\circ$
$\Phi$	1, 2, 3

m is the mass in sub- $\mu$ m-sized dust grains, p is the power which governs the decline of the surface density with increasing distance to the star ( $\Sigma \propto R^{-p}$ ), i is the inclination of the disk with respect to the line-of-sight, $\Phi$ is the artificial scaling factor for the inner disk scale height, with $\Phi = 1$ indicating hydrostatic-equilibrium models. See text for details.

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