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SUMMARY:Nonlinear interaction of tidal flows in the convective envelopes o
 f low-mass stars or giant gaseous planets - Aurelie Astoul\, University of
  Leeds
DTSTART:20220530T130000Z
DTEND:20220530T140000Z
UID:TALK174062@talks.cam.ac.uk
CONTACT:Zhao Guo
DESCRIPTION:In close exoplanetary systems\, tidal interactions are known t
 o shape the orbital architecture of the system\, modify star and planet sp
 ins\, and have an impact on the internal structure of the bodies through t
 idal heating. Most stars around which planets have been discovered are low
 -mass stars and thus feature a convective envelope\, as is also expected i
 n giant gaseous planets like Hot-Jupiter. The dissipation of tidal flows\,
  and more specifically the dissipation of tidal inertial waves (restored b
 y the Coriolis acceleration) can be particularly important in the convecti
 ve envelopes\, especially in the early stage of the life of the system. In
  parallel\, the nonlinear self-interaction of inertial waves is known to a
 ffect the structure of the background flow by triggering differential rota
 tion in convective shells\, as shown in numerical and experimental hydrody
 namical studies.\n\n In this context\, I will review and show how the addi
 tion of nonlinearities affects the tidal flow properties\, the energy and 
 angular momentum balances\, thanks to 3D hydrodynamic nonlinear simulation
 s of tides\, in an adiabatic and incompressible convective shell. Using a 
 realistic forcingto tidally excite inertial waves\, we show that cylindric
 al differential rotation still develops in our model due to the non unifor
 m deposition of angular momentum\, when shear layers (straight structures 
 where the waves are focused) are activated inside the shell. Moreover we d
 o not observe unexpected angular momentum evolution leading to the desynch
 ronisation of the bodies\, as reported in some previous simulations. I wil
 lexplain to what extent and how the emergence of differential rotation is 
 modifying the tidal dissipation rates\, prior to linear predictions. Furth
 ermore\, nonlinear self-interactions of tidal inertial waves in the newly 
 generated zonal flows can also trigger different kind of instabilities and
  resonances\, when the tidal forcing is strong enough or the viscosity low
  enough. These various interactions between tidal inertial waves and shear
 ed zonal flows reshape the energetic exchanges inside the shell\, and also
  further modifies tidal dissipation rates.
LOCATION:In Person MR14
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