3D MHD simulations of subsurface convection in OB stars

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dc.contributor University of Helsinki, Department of Physics en
dc.contributor.author Cantiello, Matteo
dc.contributor.author Braithwaite, Jonathan
dc.contributor.author Brandenburg, Axel
dc.contributor.author Del Sordo, Fabio
dc.contributor.author Käpylä, Petri
dc.contributor.author Langer, Norbert
dc.date.accessioned 2012-01-02T11:30:01Z
dc.date.available 2012-01-02T11:30:01Z
dc.date.issued 2011
dc.identifier.citation Cantiello , M , Braithwaite , J , Brandenburg , A , Del Sordo , F , Käpylä , P & Langer , N 2011 , ' 3D MHD simulations of subsurface convection in OB stars ' Proceedings of the International Astronomical Union , vol 6 , no. S272 , pp. 32-37 . DOI: 10.1017/S174392131100994X en
dc.identifier.issn 1743-9213
dc.identifier.other PURE: 10505749
dc.identifier.other PURE UUID: 5d072766-8181-4dfa-b900-ab2fc9049d5f
dc.identifier.other ArXiv: http://arxiv.org/abs/1009.4462v1
dc.identifier.other Scopus: 84856658347
dc.identifier.uri http://hdl.handle.net/10138/28870
dc.description.abstract During their main sequence evolution, massive stars can develop convective regions very close to their surface. These regions are caused by an opacity peak associated with iron ionization. Cantiello et al. (2009) found a possible connection between the presence of sub-photospheric convective motions and small scale stochastic velocities in the photosphere of early-type stars. This supports a physical mechanism where microturbulence is caused by waves that are triggered by subsurface convection zones. They further suggest that clumping in the inner parts of the winds of OB stars could be related to subsurface convection, and that the convective layers may also be responsible for stochastic excitation of non-radial pulsations. Furthermore, magnetic fields produced in the iron convection zone could appear at the surface of such massive stars. Therefore subsurface convection could be responsible for the occurrence of observable phenomena such as line profile variability and discrete absorption components. These phenomena have been observed for decades, but still evade a clear theoretical explanation. Here we present preliminary results from 3D MHD simulations of such subsurface convection. fi
dc.format.extent 6
dc.language.iso eng
dc.relation.ispartof Proceedings of the International Astronomical Union
dc.rights en
dc.subject astro-ph.SR en
dc.subject astro-ph.EP en
dc.subject 115 Astronomy, Space science en
dc.title 3D MHD simulations of subsurface convection in OB stars en
dc.title.alternative 3D MHD simulations of subsurface convection in OB stars en
dc.type Conference article
dc.identifier.doi https://doi.org/10.1017/S174392131100994X
dc.type.uri info:eu-repo/semantics/other

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