Issue 
A&A
Volume 575, March 2015



Article Number  A129  
Number of page(s)  11  
Section  Interstellar and circumstellar matter  
DOI  https://doi.org/10.1051/00046361/201424806  
Published online  11 March 2015 
Online material
Appendix A: CIRs for the case γ = 2
Our results have focused exclusively on the case of γ = 1 for the wind velocity law. Of course, other values of γ may be considered. In general, the solution for the spiral shape of the spiral will not be analytic but must be evaluated numerically. However, analytic solutions for ϕ(ξ) can be found for integer values of γ. Expected values of γ for earlytype star winds range from γ = 0.5 from the original Castor et al. (1975) paper for linedriven winds to γ ≈ 0.8 from Pauldrach et al. (1986) that augmented the initial results of Castor et al. to the γ = 1 that is typically used for the inner wind of WR stars (e.g., Schmutz et al., 1989) and then to γ ≈ 3, which has been suggested for some supergiant winds (e.g., Prinja et al., 1995).
As an example, the case of γ = 2 is provided here as a comparison case to γ = 1. In general, higher values of γ tend to increase the radial width over which the bulk of wind acceleration takes place. For example, with , the radius in the wind where the flow achieves half its terminal speed, w = 0.5, occurs at , which increases as γ becomes larger. As a case in point, for γ = 1, but for γ = 2, the value of increases to 3.4b. The net effect of this is that for our construction of the CIR spiral shape, at a given value of ω, a CIR tends to wind up at smaller radius with increasing γ, so the effective winding radius decreases with larger γ.
We need to evaluate ϕ′ for γ = 2. We start with Eq. (25) for a CIR in the equatorial plane, reproduced here: (A.1)The wind velocity is w = (1 − bξ)^{2}. Inserting w into the above expression gives (A.2)The solution for this expression is (A.3)Figure A.1 shows a comparison between these functions. There a value of r_{0}/R_{∗} = 10 is used. At most radii the value of ϕ′ is about 50% to 100% higher for γ = 2 than for γ = 1. As compared to γ = 1, the effective value of r_{0} is about half as large when γ = 2.
For the polarization one should also note that for a given optical depth of the envelope, larger γ essentially implies a relatively higher density of scatterers at small radii as compared to winds with lower γ values. Figure A.2 compares the polarization light curves for the solutions displayed in Fig. A.1: equatorial CIRs, r_{0}/R_{∗} = 10, w_{0} = 0.03, same opening angle, with η = 1, and i_{0} = 60° for both cases. The polarization is plotted as the ratio p/τ, where τ is the optical depth of the wind. As can be seen, for the selected parameters that are relevant to fast winds, the polarization per unit optical depth is similar for the two cases, but there is a slight phase shift owing to the different degrees of CIR winding. This result does not assume the same base density n_{0} for the two cases, but rather the same wind optical depth.
(For the same n_{0}, the optical depth of a γ = 2 wind is 1.6 times greater than for γ = 1.)
Fig. A.1
Comparison of the azimuth location of the CIR centroid with radius from the star. Here blue is for γ = 1, and red is for γ = 2. This example uses a wind radius of r_{0} = 10R_{∗}. The value of φ′ is generally between 50% to 100% larger for γ = 2 than for γ = 1 indicating that a spiral CIR is considerably more curved at a given radius for the higher γ case. 

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Fig. A.2
Comparison of polarization light curves for the γ = 1 and γ = 2 cases shown in the previous figure. The polarization is plotted as normalized to the wind optical depth along a radial. The case of γ = 1 produces a relatively stronger polarization signal (per unit optical depth) than in the case of γ = 2. The polarization extrema are slightly shifted in phase between the two cases. 

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© ESO, 2015
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