Corrigendum to “Elliptical instability in hot Jupiter systems” ICARUS, Volume 226, Issue 2, November–December 2013, Pages 1642–1653

A direct numerical simulation is presented of an elliptical instability observed in the laboratory within an elliptically distorted, rapidly rotating, fluid-filled cylinder (Malkus 1989). Generically, the instability manifests itself as the pairwise resonance of two different inertial modes with the underlying elliptical flow. We study in detail the simplest ‘subharmonic’ form of the instability where the waves are a complex conjugate pair and which at weakly supercritical elliptical distortion should ultimately saturate at some finite amplitude (Waleffe 1989; Kerswell 1992). Such states have yet to be experimentally identified since the flow invariably breaks down to small-scale disorder. Evidence is presented here to support the argument that such weakly nonlinear states are never seen because they are either unstable to secondary instabilities at observable amplitudes or neighbouring competitor elliptical instabilities grow to ultimately disrupt them. The former scenario confirms earlier work (Kerswell 1999) which highlights the generic instability of inertial waves even at very small amplitudes. The latter represents a first numerical demonstration of two competing elliptical instabilities co-existing in a bounded system.

Download Full-text

Tidal excitation of hydromagnetic waves and their damping in the Earth

Journal of Fluid Mechanics ◽

10.1017/s0022112094002107 ◽

1994 ◽

Vol 274 ◽

pp. 219-241 ◽

Cited By ~ 50

Author(s):

R. R. Kerswell

Keyword(s):

Growth Rate ◽

Growth Rates ◽

Outer Core ◽

Decay Rates ◽

Wave Disturbance ◽

Instability Mechanism ◽

The Earth ◽

Elliptical Instability ◽

Hydromagnetic Waves

We examine the possibility that the Earth's outer core, as a tidally distorted fluid-filled rotating spheroid, may be the seat of an elliptical instability. The instability mechanism is described within the framework of a simple Earth-like model. The preferred forms of wave disturbance are explored and a likely growth rate supremum deduced. Estimates are made of the Ohmic and viscous decay rates of such hydromagnetic waves in the outer core. Rather than a conclusive disparity of scales, we find that typical elliptical growth rates, Ohmic decay rates and viscous decay rates all have the same order for plausible core fields and core-to-mantle conductivities. This study is all the more timely considering the recent realization that the Earth's precession may also drive similar instabilities at comparable strengths in the outer core.

Download Full-text

TiO and VO broad band absorption features in the optical spectrum of the atmosphere of the hot-Jupiter HD 209458b

Astronomy and Astrophysics ◽

10.1051/0004-6361:200810355 ◽

2008 ◽

Vol 492 (2) ◽

pp. 585-592 ◽

Cited By ~ 86

Author(s):

J.-M. Désert ◽

A. Vidal-Madjar ◽

A. Lecavelier des Etangs ◽

D. Sing ◽

D. Ehrenreich ◽

...

Keyword(s):

Optical Spectrum ◽

Broad Band ◽

Band Absorption ◽

Absorption Features ◽

Hot Jupiter

Download Full-text

Hot Jupiter Variability in Eclipse Depth

The Astrophysical Journal ◽

10.1086/519374 ◽

2007 ◽

Vol 662 (2) ◽

pp. L115-L118 ◽

Cited By ~ 34

Author(s):

Emily Rauscher ◽

Kristen Menou ◽

James Y.-K. Cho ◽

Sara Seager ◽

Bradley M. S. Hansen

Keyword(s):

Hot Jupiter

Download Full-text

0.94-2.42 μm GROUND-BASED TRANSMISSION SPECTRA OF THE HOT JUPITER HD-189733b

The Astrophysical Journal ◽

10.1088/0004-637x/785/1/35 ◽

2014 ◽

Vol 785 (1) ◽

pp. 35 ◽

Cited By ~ 17

Author(s):

C. Danielski ◽

P. Deroo ◽

I. P. Waldmann ◽

M. D. J. Hollis ◽

G. Tinetti ◽

...

Keyword(s):

Transmission Spectra ◽

Hot Jupiter

Download Full-text

Tidally induced stellar oscillations: converting modelled oscillations excited by hot Jupiters into observables

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3394 ◽

2020 ◽

Vol 500 (2) ◽

pp. 2711-2731

Author(s):

Andrew Bunting ◽

Caroline Terquem

Keyword(s):

Radial Velocity ◽

Orbital Period ◽

Planetary Systems ◽

Velocity Signal ◽

Convective Flux ◽

Hot Jupiters ◽

Stellar Oscillations ◽

Orbital Periods ◽

Hot Jupiter

ABSTRACT We calculate the conversion from non-adiabatic, non-radial oscillations tidally induced by a hot Jupiter on a star to observable spectroscopic and photometric signals. Models with both frozen convection and an approximation for a perturbation to the convective flux are discussed. Observables are calculated for some real planetary systems to give specific predictions. The photometric signal is predicted to be proportional to the inverse square of the orbital period, P−2, as in the equilibrium tide approximation. However, the radial velocity signal is predicted to be proportional to P−1, and is therefore much larger at long orbital periods than the signal corresponding to the equilibrium tide approximation, which is proportional to P−3. The prospects for detecting these oscillations and the implications for the detection and characterization of planets are discussed.

Download Full-text