Figure 1: Difference between the theoretical radial velocity curves measured by the profile minimum method ( ) and the Gaussian fitting method ( ). The small difference induces a bias in the determination of the p-factor. The horizontal line is the zero velocity in the stellar rest frame. | |
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Figure 2: Pulsation velocities vs. phase. The dashed curve shows the velocity of the photospheric layer ( in the continuum), the dot-dashed curve the velocity of the layer corresponding to in the spectral center of the line and the dotted curve the gas velocity corresponding to in the line. The horizontal line is the zero velocity in the stellar rest frame. | |
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Figure 3: Radial velocity curve deduced from the theoretical line profiles by the Gaussian method together with a) the gas velocity corresponding to in the line forming region according to Eq. (1), b) the "optical layer'' velocity according to Eq. (2), c) the velocity of the photospheric layer ( in the continuum, see Eq. (3)). | |
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Figure 4: The quantity versus the phase in the case of Fig. 3a: is the gas velocity corresponding to in the line formation region according to Eq. (1), and is the radial velocity curve deduced from the theoretical line profiles by the Gaussian method. p=1.35 is the optimum value obtained from the estimator 1, as described in Sect. 4.2 | |
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Figure 5: Simulated angular diameter points deduced from Eq. (9) with . Each point is shown with its arbitrary theoretical error bar of 0.01 mas. This curve simulates interferometric observations used in the IBW method. | |
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