Show simple item record

dc.contributor.authorBarker, Adrianen
dc.date.accessioned2016-03-30T14:05:19Z
dc.date.available2016-03-30T14:05:19Z
dc.date.issued2016-06-11en
dc.identifier.citationMonthly Notices of the Royal Astronomical Society 2016en
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/254732
dc.description.abstractI present results from the first global hydrodynamical simulations of the elliptical instability in a tidally deformed gaseous planet (or star) with a free surface. The elliptical instability is potentially important for tidal evolution of the shortest-period hot Jupiters. I model the planet as a spin-orbit aligned or anti-aligned, and non-synchronously rotating, tidally deformed, homogeneous fluid body. A companion paper presented an analysis of the global modes and instabilities of such a planet. Here I focus on the non-linear evolution of the elliptical instability. This is observed to produce bursts of turbulence that drive the planet towards synchronism with its orbit in an erratic manner. If the planetary spin is initially anti-aligned, the elliptical instability also drives spin-orbit alignment on a similar time-scale as the spin synchronization. The instability generates differential rotation inside the planet in the form of zonal flows, which play an important role in the saturation of the instability, and in producing the observed burstiness. These results are broadly consistent with the picture obtained using a local Cartesian model (where columnar vortices played the role of zonal flows). I also simulate the instability in a container that is rigid (but stress-free) rather than free, finding broad quantitative agreement. The dissipation resulting from the elliptical instability could explain why the shortest-period hot Jupiters tend to have circular orbits inside about 2-3 d, and predicts spin synchronization (and spin-orbit alignment) out to about 10-15 d. However, other mechanisms must be invoked to explain tidal circularization for longer orbital periods.
dc.language.isoenen
dc.publisherOxford Academic
dc.titleNon-linear tides in a homogeneous rotating planet or star: Global simulations of the elliptical instabilityen
dc.typeArticle
dc.provenanceOA-7901
prism.endingPage956
prism.issueIdentifier1en
prism.publicationDate2016en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage939
prism.volume459en
dc.rioxxterms.funderSTFC
dc.rioxxterms.projectidST/J001570/1
dc.rioxxterms.projectidST/L000636/1
dc.rioxxterms.projectidST/K000373/1
dc.rioxxterms.projectidST/K0003259/1
dcterms.dateAccepted2016-03-22en
rioxxterms.versionofrecord10.1093/mnras/stw702en
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2016-06-11en
dc.identifier.eissn1365-2966
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idSTFC (ST/J005673/1)
pubs.funder-project-idSTFC (ST/L000636/1)
pubs.funder-project-idSTFC (ST/J001570/1)
cam.issuedOnline2016-03-28en
cam.orpheus.successThu Jan 30 12:54:35 GMT 2020 - Embargo updated*


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record