Any stream of gas flowing outward from a star, including the very rapid winds from hot, luminous stars; the intermediate- velocity, rarefied winds from stars like the sun; and the slow, dense winds from cool supergiant stars
the ejection of gas off the surface of a star. Many different types of stars, including our Sun, have stellar winds; however, a star's wind is strongest near the end of its life when it has consumed most of its fuel. (See also text in StarForm and StarDeath.)
is the flow of material from a star to the Galaxy. In the electric star the stellar wind exists as one means of the star accumulating charge from the nearly "empty" space which surrounds it. By sending electron-deficient atoms to the Galaxy the star gains electrons relative to the material it contains. From the few stellar winds that have been measured, it seems as if the mass loss increases as the square root of the luminosity. In terms of the electric star model presented here, it is tempting to think that luminosity varies as the square of the star-to-galaxy current. There is some evidence that mass loss is enhanced when a close companion is present (Hutchings).