Impact of an inhomogeneous density distribution on selected observational characteristics of circumstellar disks (Corrigendum)
University of Kiel, Institute of Theoretical Physics and Astrophysics, Leibnizstrasse 15, 24118 Kiel, Germany
e-mail: rbrauer@astrophysik.uni-kiel.de; wolf@astrophysik.uni-kiel.de
Key words: protoplanetary disks / circumstellar matter / stars: pre-main sequence / radiative transfer / dust, extinction / polarization / errata, addenda
In the legend of Fig. 7, the density contrast k needs to be 100 instead of 0.01. The x- and y-axis ticks of Figs. 8 and 10 need to be [0.3,0.5,0.7,0.8,0.95] for the mass ratio and [3.2,10,32,100] for the density contrast. However, these corrections have no influence on the results of this paper.
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Fig. 7 Radial brightness profile (left) and its standard deviation (right) of the reference and two clumpy circumstellar disks. 50 concentric rings are used for the calculation of the brightness profile. (λ = 0.726 μm, i = 0°, Mdust = 10-6 M⊙, amin = 0.005 μm and amax = 0.25 μm) |
| Open with DEXTER | |
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Fig. 8 Mean degree of polarization (left) and its standard deviation (right) dependent on mass ratio and density contrast. Each configuration is simulated with 100 different positions of clumps. (λ = 0.726 μm, i = 0°, Mdust = 10-6 M⊙, amin = 0.005 μm and amax = 0.25 μm) |
| Open with DEXTER | |
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Fig. 10 Mean degree of polarization (left) and its standard deviation (right) dependent on mass ratio and density contrast. Each configuration is simulated with 100 different positions of clumps. (λ = 0.726 μm, i = 45°, Mdust = 10-6 M⊙, amin = 0.005 μm and amax = 0.25 μm) |
| Open with DEXTER | |
© ESO, 2016