Mass Loss and Stellar Rotation

Conference Summary: Mass Loss from Stellar Clusters

Mass loss at the lowest stellar masses ⋆

We report the discovery of a jet in a [SII] image of Par-Lup3-4, a remarkable M5-type pre-main sequence object in the Lupus 3 star-forming cloud. The spectrum of this star is dominated by the emission lines commonly interpreted as tracers of accretion and outflows. Par-Lup3-4 is therefore at the very low-mass end of the exciting sources of jets. High resolution spectroscopy shows that the [SII]...

Stellar Ages from Stellar Rotation

Our ability to determine stellar ages from measurements of stellar rotation, hinges on how well we can measure the dependence of rotation on age for stars of different masses. Rotation periods for stars in open clusters are essential to determine the relations between stellar age, rotation, and mass (color). Until recently, ambiguities in v sin i data and lack of cluster membership information,...

Asteroseismology and Stellar Rotation

We discuss how the structure and oscillation frequencies of delta Scuti stars are aaected by fast rotation. We investigate the impact of these changes on our interpretation of observed frequencies used in an as-teroseismic analysis. We nd that, to rst order, frequency ratios between pairs of radial modes are not sensitive to rotation. However, for non-radial modes we nd that second-order terms ...

Stellar evolution with rotation VI: The Eddington and Ω–limits, the rotational mass loss for OB and LBV stars

Several properties of massive stars with large effects of rotation and radiation are studied. For stars with shellular rotation, i.e. stars with a constant angular velocity Ω on horizontal surfaces (cf. Zahn 1992), we show that the equation of stellar surface has no significant departures with respect to the Roche model; high radiation pressure does not modify this property. Also, we note that ...