Circumstellar disks around Herbig Be stars | Astronomy & Astrophysics (A&A)

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This article has an erratum: [https://doi.org/10.1051/0004-6361/200810401e]

Table 5:

Grain properties in the disks¹.
Name	Midplane	Surface
	grains	grains
MWC 137	SM $a_{\max}=1$ cm	SM $a_{\max}=1~\mu$ m
R Mon	SM $a_{\max}=1$ cm	86% graphite $^{100\%}_{50\%}$ $a_{\max}=1~\mu$ m
MWC 1080	SM $a_{\max}=1$ cm	SM $a_{\max}=100~\mu$ m
MWC 297	SM $a_{\max}=1$ cm	SM $a_{\max}=1~\mu$ m
LKHa 215	SM $a_{\max}=1$ cm	SM $a_{\max}=100~\mu$ m
Z CMa	SM $a_{\max}=1$ cm	60% graphite $^{100\%}_{50\%}$ $a_{\max}=1~\mu$ m

¹ The index of the power-law grain-size distribution is fixed (p=3.5). As a first step, we assumed the standard mixture (SM: 86% silicates/14% graphite) in the midplane and surface layers in all the sources. In the cases of R Mon and Z CMa, we needed to change the dust composition in the surface to fit the SED. The range of allowed values are indicated (small figures) in the Table. See Sect. 5.7 for a detailed discussion of the uncertainties.

Source LaTeX | All tables | In the text

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