Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008arep...52..237r&link_type=abstract
Astronomy Reports, Volume 52, Issue 3, pp.237-246
Astronomy and Astrophysics
Astronomy
2
97.10.Sj, 97.30.-B, 95.85.Kr, 97.10.Kc, Pulsations, Oscillations, And Stellar Seismology, Variable And Peculiar Stars, Visible, Stellar Rotation
Scientific paper
We have studied the variability of the Hell λλ 4686 and 5411 Å H β, and H α lines in the spectrum of the pulsating star HD 93521. All these line profiles display the same variability pattern relative to the average profiles: a sinusoidal wave that moves systematically from the short-to the long-wavelength wing of the profile. This variability is due to non-radial pulsations. To study the pulsation movements and stratification of the radial velocity in the atmosphere of HD 93521, we analyzed the variability of the radial velocities measured individually for the blue and red halves of the absorption profile at the half-level of the line intensity. The periods and amplitudes of this radial-velocity variability are different for different lines and are well correlated with their central depths. In the transition from weak to strong lines (i.e., from lower to upper layers of the atmosphere), the period of the radial-velocity variations measured using both halves of the absorption profile increases, while its amplitude decreases. When the morphology and variability of photospheric and wind-driven lines are compared, it is clear that the variability of their absorption components is due to the same process—non-radial pulsations. In this way, the non-radial pulsations partly affect the variability of the stellar wind. The effect of the stellar wind on the profiles of strong lines is observed as a variable absorption feature that moves along the profiles synchronous with the axial rotation of the star.
Panchuk Vladimir E.
Rzaev Kh. A.
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