Thermohaline mixing in low-mass giants: RGB and beyond

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dc.creatorCantiello, M.
dc.creatorHoekstra, H.
dc.creatorLanger, N.
dc.creatorPoelarends, A. J. T.
dc.date2007-08-31
dc.date.accessioned2026-07-07T10:57:17Z
dc.date.available2026-07-07T10:57:17Z
dc.descriptionThermohaline mixing has recently been proposed to occur in low mass red giants, with large consequence for the chemical yields of low mass stars. We investigate the role of thermohaline mixing during the evolution of stars between 1 Msun and 3 Msun. We use a stellar evolution code which includes rotational mixing and internal magnetic fields. We confirm that thermohaline mixing has the potential to destroy most of the helium 3 which is produced earlier on the main sequence during the red giant stage, in stars below 1.5Msun. We find this process to continue during core helium burning and beyond. We find rotational and magnetic mixing to be negligible compared to the thermohaline mixing in the relevant layers, even if the interaction of thermohaline motions with the differential rotation may be essential to establish the time scale of thermohaline mixing in red giants.
dc.descriptionProceedings of the Conference "Unsolved problems in stellar physics" - Cambridge, July 2007
dc.identifierhttps://arxiv.org/abs/0708.4384
dc.identifierhttp://arxiv.org/abs/0708.4384
dc.identifierAIPConf.Proc.948:73-77,2007
dc.identifierdoi:10.1063/1.2819014
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/186700
dc.subjectAstrophysics
dc.titleThermohaline mixing in low-mass giants: RGB and beyond
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