Stellar winds from hot low-mass stars

摘要: Stellar winds appear as a persistent feature of hot stars, irrespective their wide range different luminosities, masses, and chemical composition. Among the massive Wolf–Rayet types show considerably stronger mass loss than O stars. low-mass stellar are seen at central stars planetary nebulae, where again hydrogen-deficient much those with “normal” We also studied mass-loss from few extreme helium sdOs. Their rate roughly follows same proportionality luminosity to power 1.5 This relation marks lower limit for all kinds, provides evidence that radiation pressure on spectral lines is basic mechanism work. For certain classes rates lie significantly above this relation, reasons not yet fully understood. Mass may affect evolution, by reducing envelope mass, can easily prevent diffusion establishing atmospheric abundance patterns. In close binary systems, feed accretion onto companion.