Fig. 2.
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Range of radial velocities between Mercury and the Sun as a function of the true anomaly angle. The right vertical axis shows the amount of wavelength shift in the solar He I 58.4 nm emission by the Doppler shift due to Mercury’s radial motion. Two lines at ±8.00 × 10−4 nm show the line width of the solar He I 58.4 nm emission estimated by Kumar (1976) and the corresponding velocities.
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