Stellar wind

It is distinguished from the bipolar outflows characteristic of young stars by being less collimated, although stellar winds are not generally spherically symmetric.

These winds are understood to be driven by radiation pressure on dust condensing in the upper atmosphere of the stars.

[citation needed] Massive stars of types O and B have stellar winds with lower mass loss rates (

Such winds are driven by radiation pressure on the resonance absorption lines of heavy elements such as carbon and nitrogen.

These winds consist mostly of high-energy electrons and protons (about 1 keV) that are able to escape the star's gravity because of the high temperature of the corona.

This image shows the wind from the star LL Orionis generating a bow shock (the bright arc) as it collides with material in the surrounding Orion Nebula .
In planetary nebula NGC 6565 , a cloud of gas was ejected from the star after strong stellar winds. [ 8 ]