Free Access
Volume 576, April 2015
Article Number A84
Number of page(s) 13
Section Interstellar and circumstellar matter
Published online 02 April 2015

Online material

Appendix A: Individual set of observations

thumbnail Fig. A.1

All three AMBER observations of HD 163296 with spectral resolution of 12 000. The three columns show the observed intereferometric results from 2012 May 11 (left), 2012 May 12 (middle), and 2012 June 04 (right). Shown from top to bottom are wavelength dependence of flux, visibilities, wavelength-differential phases (for better visibility, the differential phases of the first and last baselines are shifted by +50° and −50°, respectively), and closure phase observed at projected baselines as shown in the plot. The wavelength scale at the bottom is corrected to the local standard of rest. The typical visibilities, differential, and closure phases errors are ±5%, 5°, and 15°.

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Appendix B: Pure line visibilities

thumbnail Fig. B.1

Comparison of the observed and modelled pure Brγ line visibilities of our AMBER observation of HD 163296. From top to bottom: wavelength dependence of flux, visibilities of the first, second, and third baseline. In each visibility panel: (1) the observed total visibilities (red, green, blue, as in Fig. 1); (2) the observed continuum-compensated pure Brγ line visibilities (pink), and the modelled pure Brγ line visibilities (black; model MW6, Table 3) are shown.

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Appendix C: Examples of computed disc wind models

thumbnail Fig. C.1

Same as Fig. B.1 (left panel) and Fig. 2 (right panel) but for model MW26 (see Table 3).

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thumbnail Fig. C.2

Same as Fig. B.1 (left panel) and Fig. 2 (right panel) but for model MW47 (see Table 3).

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Appendix D: Examples of computed hybrid models: disc wind plus magnetosphere

Appendix D.1: The magnestosphere

A full description of the model employed here can be found in Tambovtseva et al. (2014). Here, only a brief description of the main model parameters is presented.

Our model considers a compact, disc-like rotating magnetosphere of height hm through which free-falling gas reaches the stellar surface at some altitude near the magnetic pole. The gas rotational velocity component (u) is described by (D.1)where U0 is the rotational velocity of the gas at the magnetic poles, r is the distance from the star, and p is a parameter. Finally, we assume a dependence of the electron temperature (Te) of (D.2)where r1 = ((rR) /R)q, Te(R) is the temperature of the gas near the stellar surface, and q is a parameter.

Table D.1

Magnetosphere model parameters

thumbnail Fig. D.1

Same as Fig. B.1 (left panel) and Fig. 2 (right panel) but for the hybrid model MW6+MS6a (see Tables 3 and D.1).

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In our hybrid model, the magnetosphere is equivalent to a point source at our interferometer baselines. Thus, it accounts for the compact and unresolved Brγ emission, whereas the disc wind component is responsible of the resolved Brγ emission.

Because of the spread on the measured acc values, and the large uncertainties in measuring this quantity (~20%), an average value of 1 × 10-7 M yr-1 was assumed in our magnetosphere model.

© ESO, 2015

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