Nonlinear Tides in Exoplanet Host Stars

Details Nonlinear Tides in Exoplanet Host Stars Nonlinear Tides in Exoplanet Host Stars

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.1006a&link_type=abstract

American Astronomical Society, ESS meeting #2, #10.06

Astronomy and Astrophysics

Astronomy

Scientific paper

Dissipation of the tide raised in the host star by a planet may lead to orbital circularization as well as spin up of the star and decay of the planet's orbit. Previous theoretical investigations have computed the tidally-induced fluid flow in the star using the linear approximation in which nonlinear terms in the fluid equation were ignored. Dissipation and secular evolution were then computed using standard heat diffusion in radiative zones or turbulent viscosity from eddies in convection zones to compute the effective tidal lag angle.
We have extended the theory of tidally-induced fluid motion to include leading order nonlinear effects due to wave-wave interactions and nonlinear tidal forces. Results are presented for the case of a Sun-like star perturbed by a planetary mass companion. We find that the linear tide so often assumed in previous studies is unstable in large ranges of parameter space, and causes gravity waves in the radiative zone to grow exponentially on short timescales. The resulting turbulent state may have larger dissipation rate than the linear tide case in some circumstances, with a corresponding increase in orbital decay and circularization. We present numerical results for close in exoplanets, contrasting linear with nonlinear theory.

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