Confirmation of bistable stellar differential rotation profiles

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dc.contributor Aalto-yliopisto fi
dc.contributor Aalto University en
dc.contributor.author Käpylä, P.J.
dc.contributor.author Käpylä, M.J.
dc.contributor.author Brandenburg, A.
dc.date.accessioned 2018-08-01T13:31:40Z
dc.date.available 2018-08-01T13:31:40Z
dc.date.issued 2014
dc.identifier.citation Käpylä , P J , Käpylä , M J & Brandenburg , A 2014 , ' Confirmation of bistable stellar differential rotation profiles ' ASTRONOMY AND ASTROPHYSICS , vol 570 , A43 . DOI: 10.1051/0004-6361/201423412 en
dc.identifier.issn 0004-6361
dc.identifier.issn 1432-0746
dc.identifier.other PURE UUID: 9e6ac62a-0eef-4c34-8157-ae47e7d6cd2d
dc.identifier.other PURE ITEMURL: https://research.aalto.fi/en/publications/confirmation-of-bistable-stellar-differential-rotation-profiles(9e6ac62a-0eef-4c34-8157-ae47e7d6cd2d).html
dc.identifier.other PURE LINK: http://www.aanda.org/articles/aa/abs/2014/10/aa23412-14/aa23412-14.html
dc.identifier.other PURE FILEURL: https://research.aalto.fi/files/26498454/aa23412_14.pdf
dc.identifier.uri https://aaltodoc.aalto.fi/handle/123456789/32859
dc.description VK: resolve; Karhunen, J.; ReSoLVE
dc.description.abstract Context. Solar-like differential rotation is characterized by a rapidly rotating equator and slower poles. However, theoretical models and numerical simulations can also result in a slower equator and faster poles when the overall rotation is slow. Aims. We study the critical rotational influence under which differential rotation flips from solar-like (fast equator, slow poles) to an anti-solar one (slow equator, fast poles). We also estimate the non-diffusive (Λ effect) and diffusive (turbulent viscosity) contributions to the Reynolds stress. Methods. We present the results of three-dimensional numerical simulations of mildly turbulent convection in spherical wedge geometry. Here we apply a fully compressible setup which would suffer from a prohibitive time step constraint if the real solar luminosity was used. To avoid this problem while still representing the same rotational influence on the flow as in the Sun, we increase the luminosity by a factor of roughly 106 and the rotation rate by a factor of102. We regulate the convective velocities by varying the amount of heat transported by thermal conduction, turbulent diffusion, and resolved convection. Results. Increasing the efficiency of resolved convection leads to a reduction of the rotational influence on the flow and a sharp transition from solar-like to anti-solar differential rotation for Coriolis numbers around 1.3. We confirm the recent finding of a large-scale flow bistability: contrasted with running the models from an initial condition with unprescribed differential rotation, the initialization of the model with certain kind of rotation profile sustains the solution over a wider parameter range. The anti-solar profiles are found to be more stable against perturbations in the level of convective turbulent velocity than the solar-type solutions. Conclusions. Our results may have implications for real stars that start their lives as rapid rotators implying solar-like rotation in the early main-sequence evolution. As they slow down, they might be able to retain solar-like rotation for lower Coriolis numbers, and thus longer in time, before switching to anti-solar rotation. This could partially explain the puzzling findings of anti-solar rotation profiles for models in the solar parameter regime. en
dc.format.extent 10
dc.format.mimetype application/pdf
dc.language.iso en en
dc.relation.ispartofseries ASTRONOMY AND ASTROPHYSICS en
dc.relation.ispartofseries Volume 570 en
dc.rights openAccess en
dc.title Confirmation of bistable stellar differential rotation profiles en
dc.type A1 Alkuperäisartikkeli tieteellisessä aikakauslehdessä fi
dc.description.version Peer reviewed en
dc.contributor.department Centre of Excellence Research on Solar Long-Term Variability and Effects, ReSoLVE
dc.subject.keyword Astrophysics - Galaxy Astrophysics
dc.subject.keyword Astrophysics - Solar and Stellar Astrophysics
dc.identifier.urn URN:NBN:fi:aalto-201808014260
dc.identifier.doi 10.1051/0004-6361/201423412
dc.type.version publishedVersion


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