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. ^{[

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Stellar wind (disambiguation)bow shockOrion Nebulaupper atmospherebipolar outflowscollimatedmain-sequencered giantssupergiantsasymptotic giant branchradiation pressureT Tauri starsstellar wind bubblesplanetary nebulaNGC 6565G-type starscoronasolar windelectronsprotonsgravitytemperaturewhite dwarfssupernovaeCosmic rayCosmic windPlanetary windColliding-wind binaryPulsar wind nebulaGalactic superwindSuperwindKlein, R. I.BibcodeFormationAccretionMolecular cloudBok globuleYoung stellar objectProtostarPre-main-sequenceHerbig Ae/BeT TauriHerbig–Haro objectHayashi trackHenyey trackEvolutionMain sequenceRed-giant branchHorizontal branchRed clumppost-AGBsuper-AGBBlue loopProtoplanetaryWolf–Rayet nebulaPG1159Dredge-upInstability stripLuminous blue variableStellar populationSupernovaSuperluminousHypernovaClassificationSubdwarfSubgiantYellowBright giantSupergiantHypergiantCarbonWhite dwarfChemically peculiarHe-weakBariumLambda BoötisTechnetiumHeliumExtremeBlue stragglerRemnantsCompact starParker's starHelium planetNeutronRadio-quietPulsarBinaryMagnetarStellar black holeX-ray binaryBursterHypotheticalBlue dwarfBlack dwarfExoticElectroweakStrangePlanckDark-energyQuasi-starGravastarThorne–Żytkow objectBlitzarWhite holeNucleosynthesisDeuterium burningLithium burningProton–proton chainCNO cycleHelium flashTriple-alpha processAlpha processC burningNe burningO burningSi burnings-processr-processp-processSymbioticRemnantLuminous red novaMicronovaStructureConvection zoneMicroturbulenceOscillationsRadiation zoneAtmospherePhotosphereStarspotChromosphereStellar coronaAlfvén surfaceBubbleBipolar outflowAccretion diskProtoplanetary diskProplydAsteroseismologyHelioseismologyCircumstellar dustCosmic dustCircumstellar envelopeEddington luminosityKelvin–Helmholtz mechanismDesignationDynamicsEffective temperatureLuminosityKinematicsMagnetic fieldAbsolute magnitudeMetallicityRotationStarlightVariablePhotometric systemColor indexHertzsprung–Russell diagramColor–color diagramStrömgren sphereKraft breakStar systemsContactCommon envelopeEclipsingClusterGlobularPlanetary systemSolar eclipseSolar radio emissionSolar SystemSunlightPole starCircumpolarConstellationAsterismMagnitudeApparentExtinctionPhotographicRadial velocityProper motionParallaxPhotometric-standardProper namesArabicChineseExtremesMost massiveHighest temperatureLowest temperatureLargest volumeSmallest volumeBrightestHistorical brightestMost luminous