Variations of the stellar wind in early-B hypergiants.

Details Variations of the stellar wind in early-B hypergiants. Variations of the stellar wind in early-B hypergiants.

Feb 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...318..819r&link_type=abstract

Astronomy and Astrophysics, v.318, p.819-834

Astronomy and Astrophysics

Astrophysics

29

Stars: Early-Type, Stars: Supergiants, Stars: Mass Loss, Stars: Individual: Zeta1 Sco, Stars: Individual: Hd 169454, Stars: Individual: Hd 190603

Scientific paper

With our fiber-linked echelle spectrograph we monitored three early-B hypergiants with high dispersion and good coverage in time. The program stars ζ^1^ Sco (HD 152236), HD 169454, and HD 190603 were observed over periods of several months in several seasons. In the years 1990 to 1994, we covered the wavelength range from 4000Å to 6740Å and in 1995 from 3450Å to 8620Å, respectively. Typically one spectrum of each object was taken every one or two nights. We found the P Cygni-type profiles of all objects to be variable, both in the emission and in the absorption. Blue-shifted variable absorption features can be seen in many lines. These features are particularly clear in the Feiiiλλ5127, 5156 lines. They can be traced from photospheric velocities to approximately -200km/s. We find radial-velocity variations of about 20km/s in the cores of photospheric lines. These variations have typical time scales of weeks. They show a time delay and a velocity shift between different lines. We interpret this delay as the propagation of disturbances through the innermost layers of the wind. These perturbations originate in the photosphere or the sub-photosphere. The variability of discrete absorption components (DACs) of P Cygni-type profiles can be modeled assuming density perturbations of the order of 10% at the base of the wind. The outward propagation of these perturbations can explain the observed variations. The perturbations move with a velocity law that is slower (β=2.5) than that of the ambient wind (β=1.5). The absorption lines show pulsation-like radial-velocity variations with a period of about 12 days. These variations last a few cycles before becoming irregular. Integrating the radial-velocity curve, we derive radius variations of the order of 10% of the stellar radius. These radius variations are correlated with the emission-line variability. The photometric data also indicate possible radial pulsations with this amplitude. The mass-loss rates of the stars derived from the Balmer-emission components are between 2.7 and 6.3x10^-6^Msun_/yr.

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