On the origin of microturbulence in hot stars

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dc.creatorCantiello, M.
dc.creatorLanger, N.
dc.creatorBrott, I.
dc.creatorde Koter, A.
dc.creatorShore, S. N.
dc.creatorVink, J.
dc.creatorVoegler, A.
dc.creatorYoon, S. -C.
dc.date2008-10-15
dc.date.accessioned2026-07-07T12:43:16Z
dc.date.available2026-07-07T12:43:16Z
dc.descriptionWe present results from the first extensive study of convection zones in the envelopes of hot massive stars, which are caused by opacity peaks associated with iron and helium ionization. These convective regions can be located very close to the stellar surface. Recent observations of microturbulence in massive stars from the VLT-Flames survey are in good agreement with our predictions concerning the occurrence and the strength of sub-surface convection in hot stars. We argue further that convection close to the surface may trigger clumping at the base of the stellar wind of massive stars.
dc.descriptionto appear in Comm. in Astroseismology - Proceedings of the 38th LIAC/HELAS-ESTA/BAG, 2008
dc.identifierhttps://arxiv.org/abs/0810.2546
dc.identifierhttp://arxiv.org/abs/0810.2546
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/220361
dc.subjectAstrophysics
dc.titleOn the origin of microturbulence in hot stars
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