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SUMMARY:Complex tidal flow interactions in stellar and planetary convectiv
 e envelopes - Aurélie Astoul (University of Leeds)
DTSTART:20230512T114500Z
DTEND:20230512T124500Z
UID:TALK198577@talks.cam.ac.uk
CONTACT:Paras Vadher
DESCRIPTION:In close star/star or star/planet systems\, tidal interactions
  are known to shape the orbital architecture of the system\, and modify th
 e star and planet spins. Most stars around which planets have been discove
 red are low-mass solar-type stars\, and thus feature a magnetised and ofte
 n differentially-rotating convective envelope\, as is also expected in gia
 nt gaseous planets. The dissipation of tidal flows\, and more specifically
  the dissipation of inertial waves (restored by the Coriolis acceleration)
  is of particular importance in the convective envelopes\, especially in t
 he early stages of the life of an exoplanetary system. In parallel\, the n
 on-linear self-interactions of inertial waves are able to trigger differen
 tial rotation in convective shells in the form of axisymmetric zonal flows
 . In turn\, linear numerical studies have shown that differential rotation
  can strongly affect the properties of inertial waves\, namely their propa
 gation and the dissipation of their kinetic energy.\n\nIn this context\, I
  will present our recent results of (magneto-)hydrodynamicalnon-linear num
 erical simulations of tidally-forced inertial waves\, in 3D spherical conv
 ective shells. The emerging zonal flow strength and structure largely depe
 nd on the viscosity\, tidal forcing amplitude and frequency. When strong\,
  these flows deeply modify tidal dissipation rates from prior linear predi
 ctions. Moreover\, we also find evidences of strong wave/wave and wave/zon
 al flow interactions leading to parametric and shear flow instabilities du
 e to corotation resonances (when the Doppler-shifted frequency vanishes). 
 Therefore\, I will discuss to what extent these various non-linear effects
  disrupt the linear predictions for tides along the permissible forcing fr
 equency range and for various viscosities\, tidal amplitudes and size of t
 he convective shells which are representative of the convective envelopes 
 of low-mass stars and giant gaseous planets.
LOCATION:LR12
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