$\mathsf{\alpha}$ Eridani: rotational distortion, stellar and circumstellar activity

Abstract

We explore the geometrical distortion and the stellar and circumstellar activity of α Eri (HD 10144), the brightest Be star in the sky. We present a thorough discussion of the fundamental parameters of the object for an independent determination of its rotational distortion. We used stellar atmosphere models and evolutionary tracks calculated for fast rotating early-type stars. If the star is a rigid rotator, its angular velocity rate is Ω/Ω c 0.8, so that its rotational distortion is smaller than the one inferred from recent interferometric measurements. We then discuss the stellar surface activity using high resolution and high S/N spectroscopic observations of He i and Mg ii lines, which concern a period of Hα line emission decline. The variations in the He i lines are interpreted as due to non-radial pulsations. Time series analysis of variations was performed with the cleanest algorithm, which enabled us to detect the following frequencies: 0.49, 0.76, 1.27 and 1.72 c/d and pulsation degrees ∼ (3−4) for ν = 0.76 c/d; ∼ (2−3) for ν = 1.27 c/d and ∼ (3−4) for ν = 1.72 c/d. The study of the absolute deviation of the He i λ6678 Å spectral line revealed mass ejection between 1997 and 1998. We conclude that the lowest frequency found, ν = 0.49 c/d, is due to the circumstellar environment, which is present even at epochs of low emission in the wings of He i λ6678 Å and Mg ii λ4481 Å line profiles, as well as during nearly normal aspects of the Hα line. This suggests that there may be matter around the star affecting some spectral regions, even though the object displays a B-normal like phase. The long-term changes of the Hα line emission in α Eri are studied. We pay much attention to the Hα line emission at the epoch of interferometric observations. The Hα line emission is modeled and interpreted in terms of varying structures of the circumstellar disc. We conclude that during the epoch of interferometric measurements there was enough circumstellar matter near the star to produce λ2.2 µm flux excess, which could account for the overestimated stellar equatorial angular diameter. From the study of the latest B Be phase transition of α Eri we concluded that the Hα line emission formation regions underwent changes so that: a) the low Hα emission phases are characterized by extended emission zones in the circumstellar disc and a steep outward matter density decline; b) during the strong Hα emission phases the emitting regions are less extended and have a constant density distribution. The long-term variations of the Hα line in α Eri seem to have a 14-15 year cyclic B Be phase transition. The disc formation time scales, interpreted as the periods during which the Hα line emission increases from zero to its maximum, agree with the viscous decretion model. On the other hand, the time required for the disc dissipation ranges from 6 to 12 years which questions the viscous disc model.

Fundamental parameters of B supergiants from the BCD system

“…The present calibration can then provide a first step for the interpretation of spectra emitted by rotating early-type objects, as already shown in Levenhagen et al (2003); Neiner et al (2003); Zorec et al (2005);Vinicius et al (2006);Frémat et al (2006); Martayan et al (2006Martayan et al ( , 2007; Floquet et al (2000Floquet et al ( , 2002.…”

“…objects whose atmospheres can be modeled in the framework of hydrostatic and radiative equilibrium approximations. However, since both the photospheric and the circumstellar components of the BD are spectroscopically well separated, it can also be used to study some "peculiar" objects, like: i) Be stars (Divan & Zorec 1982;Zorec 1986;Zorec & Briot 1991;Chauville et al 2001;Zorec et al 2005;Vinicius et al 2006); ii) objects with the B[e] phenomenon (Cidale et al 2001); iii) chemically peculiar stars (He-W group) (Cidale et al 2007). …”

The environment of the fast rotating star Achernar

“…This strong flattening could not be explained by the commonly adopted stellar rotation models, and two possibilities were proposed to account for it: differential rotation (Jackson et al 2004), and a residual circumstellar disk (Carciofi et al 2008). By studying the time variation of Hα line profiles, Vinicius et al (2006) showed that a weak but measurable emission (relative to a reference spectra) was detectable at the epoch of the VLTI/VINCI observations; this supports the hypothesis of a residual disk.…”

Kinematics and geometrical study of the Be stars 48 Persei andψPersei with the VEGA/CHARA interferometer

“…Previous spectrally resolved interferometric observations (Meilland et al 2007a,b) and spectroscopic follow-ups (Miroshnichenko et al 2003;Vinicius et al 2006) showed evidence that the kinematics in the equatorial plan was dominated by rotation. Thus, because of the lack of available measurements for our targets and the introduction of additional parameters needed to take into account the incoherent scattering effect, we decided to neglect the expansion in the equatorial disk (i.e., V 0 = V ∞ = 0 km s −1 ).…”