2017
DOI: 10.1051/0004-6361/201629932
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Revealing the structure of the outer disks of Be stars

Abstract: Context. The structure of the inner parts of Be star disks ( 20 stellar radii) is well explained by the viscous decretion disk (VDD) model, which is able to reproduce the observable properties of most of the objects studied so far. The outer parts, on the other hand, are not observationally well-explored, as they are observable only at radio wavelengths. A steepening of the spectral slope somewhere between infrared and radio wavelengths was reported for several Be stars that were previously detected in the rad… Show more

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Cited by 54 publications
(85 citation statements)
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References 68 publications
(114 reference statements)
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“…For the less massive disks witḣ M ≤ 10 −8 M yr −1 the value of the same slope parameter within the same region is approximately 3.125. This agrees with observational results of Klement et al (2017), who determine the values of the disk midplane density slope parameter between approximately 3.0 and 3.5 for the Be stars' disks that are in a steady state. They also predict that disks with this parameter higher than 3.5 should correspond to disks that are in the process of formation, and that disks with this parameter lower than 3 are in the process of dissipation; the variations of the values of the slope parameter in the case of very massive disks indicate that these processes occur up to a certain distance (see Sect.…”
Section: Discussionsupporting
confidence: 91%
“…For the less massive disks witḣ M ≤ 10 −8 M yr −1 the value of the same slope parameter within the same region is approximately 3.125. This agrees with observational results of Klement et al (2017), who determine the values of the disk midplane density slope parameter between approximately 3.0 and 3.5 for the Be stars' disks that are in a steady state. They also predict that disks with this parameter higher than 3.5 should correspond to disks that are in the process of formation, and that disks with this parameter lower than 3 are in the process of dissipation; the variations of the values of the slope parameter in the case of very massive disks indicate that these processes occur up to a certain distance (see Sect.…”
Section: Discussionsupporting
confidence: 91%
“…Finally, we comment on the disk structure near the central star that is suggested by some results of the present paper. Detailed accounts of successful representations of the observed emission in the Hα line of Be stars and of the continuum energy distribution from the far-UV to the IR, as well as of the polarization in the visible spectral range, are given in a series of rather recent papers and references therein (Araya et al 2017;Arcos et al 2017;Klement et al 2017;Marr et al 2018). In all these studies, the physical structure of the CE of Be stars is studied in the frame of an axisymmetric quasi-Keplerian disk in hydrostatic equilibrium in the vertical axis, where the scale height H is proportional to R 3/2 T 1/2 and R represents the equatorial radius of the disk and T is its local temperature.…”
Section: Discussionmentioning
confidence: 99%
“…where Λ = 1/(1 −r − 1 2 out ), withr out = R out /R eq , is a number usually just slightly larger than 1, as R out R eq . The steadystate AM loss rate, therefore, depends very little (through the factor Λ) on the outer radius of the disc, whose value is poorly known for a few Be stars, and completely unknown for most (Klement et al 2017). In the simulations presented in this work, we have setr out = 1000.…”
Section: Model Descriptionmentioning
confidence: 99%