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{{About|gas ejected from the atmosphere of stars}} | |||
A '''stellar wind''' is a flow of neutral or charged gas ejected from the [[stellar atmosphere|upper atmosphere]] of a [[star]]. It is distinguished from the [[bipolar outflow]]s characteristic of young stars by being less [[collimated]], although stellar winds are not generally spherically symmetric. | |||
Different [[stellar classification|types]] of stars have different types of stellar winds. | |||
Post-[[main sequence|main-sequence]] [[star]]s nearing the ends of their lives often eject large quantities of mass in massive (<math> \scriptstyle \dot{M} > 10^{-3}</math> solar masses per year), slow (v = 10 km/s) winds. These include [[red giant]]s and [[Red supergiants|supergiants]], and [[asymptotic giant branch]] stars. These winds are likely to be driven by [[radiation pressure]] on [[Cosmic dust|dust]] condensing in the upper atmosphere of the stars. | |||
Massive stars of [[stellar classification|types]] [[O star|O]] and [[B V star|B]] have stellar winds with lower mass loss rates (<math>\scriptstyle \dot{M} < 10^{-6}</math> solar masses per year) but very high velocities (v > 1–2000 km/s). Such winds are driven by radiation pressure on the resonance absorption lines of heavy elements such as carbon and nitrogen.<ref>{{cite journal| bibcode=1975ApJ...195..157C| last= Castor| first=J.| coauthors=Abbott, D. C., & [[Richard Klein (astronomer)|Klein, R. I.]]| title=Radiation-driven winds in Of stars| year=1975| journal=Astrophys. J.| volume=195| pages=157–174| doi=10.1086/153315}}</ref> These high-energy stellar winds blow [[stellar wind bubble]]s. | |||
[[G-type main-sequence star|G-type stars]] like the [[Earth|Earth's]] [[Sun]], have a wind driven by their hot, magnetized [[corona]]. The Sun's wind is called the [[solar wind]]. These winds consist mostly of high-energy [[electrons]] and [[proton]]s (about 1 [[electron volt|keV]]) that are able to escape the star's [[gravity]] because of the high [[temperature]] of the [[corona]]. | |||
Stellar winds from [[main sequence|main-sequence]] [[star]]s do not strongly influence the evolution of lower mass stars such as the Sun. However, for more massive stars such as O stars, the mass loss can result in a star shedding as much as 50% of its mass whilst on the main sequence: this clearly has a significant impact on the later stages of evolution. The influence can even be seen for intermediate mass stars, which will become [[white dwarf]]s at the ends of their lives rather than exploding as [[supernova]]e only because they lost enough mass in their winds. | |||
==See also== | |||
{{Portal|Space}} | |||
* [[Solar wind]] | |||
* [[Cosmic ray]] | |||
==References== | |||
<references/> | |||
{{Star}} | |||
{{DEFAULTSORT:Stellar Wind}} | |||
[[Category:Stellar astronomy]] | |||
Revision as of 09:07, 2 February 2014
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A stellar wind is a flow of neutral or charged gas ejected from the upper atmosphere of a star. It is distinguished from the bipolar outflows characteristic of young stars by being less collimated, although stellar winds are not generally spherically symmetric.
Different types of stars have different types of stellar winds.
Post-main-sequence stars nearing the ends of their lives often eject large quantities of mass in massive ( solar masses per year), slow (v = 10 km/s) winds. These include red giants and supergiants, and asymptotic giant branch stars. These winds are likely to be driven by radiation pressure on dust condensing in the upper atmosphere of the stars.
Massive stars of types O and B have stellar winds with lower mass loss rates ( solar masses per year) but very high velocities (v > 1–2000 km/s). Such winds are driven by radiation pressure on the resonance absorption lines of heavy elements such as carbon and nitrogen.[1] These high-energy stellar winds blow stellar wind bubbles.
G-type stars like the Earth's Sun, have a wind driven by their hot, magnetized corona. The Sun's wind is called the solar wind. 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.
Stellar winds from main-sequence stars do not strongly influence the evolution of lower mass stars such as the Sun. However, for more massive stars such as O stars, the mass loss can result in a star shedding as much as 50% of its mass whilst on the main sequence: this clearly has a significant impact on the later stages of evolution. The influence can even be seen for intermediate mass stars, which will become white dwarfs at the ends of their lives rather than exploding as supernovae only because they lost enough mass in their winds.
See also
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References
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