Turbulent convection is thought to act as an effective viscosity ($ν_E$) in damping tidal flows stars and giant planets. However, the efficiency of this mechanism has long been debated, particularly regime fast tides, when frequency ($ω$) exceeds turnover dominant convective eddies ($ω_c$). We present results hydrodynamical simulations study interaction between a small patch zone. These build upon our prior work by simulating more turbulent larger horizontal boxes, here we explore wider...

Tidal interactions are important in driving spin and orbital evolution planetary stellar binary systems, but the fluid dynamical mechanisms responsible remain incompletely understood. One key mechanism is interaction between tidal flows convection. Turbulent convection thought to act as an effective viscosity damping large-scale flows, there a long-standing controversy over efficiency of this when frequency exceeds turnover dominant convective eddies. This high regime relevant for many...

Abstract Recent work suggests that inwardly propagating internal gravity waves (IGWs) within a star can be fully converted to outward magnetic if they encounter sufficiently strong field. The resulting dissipate as propagate regions with lower Alfvén velocity. While tidal forcing is known excite IGWs, this conversion and subsequent damping of have not been explored dissipation mechanism. In particular, stars fields could tidally excited waves, yielding the same evolution previously studied...

ABSTRACT The leading theoretical paradigm for the Sun’s magnetic cycle is an αω-dynamo process, in which a combination of differential rotation and turbulent, helical flows produces large-scale field that reverses every 11 yr. Most αω solar dynamo models rely on tachocline to generate strong toroidal field. most problematic part such then production poloidal field, via process known as α-effect. Whilst this usually attributed small-scale convective motions under influence rotation,...

Recent work suggests that inwardly propagating internal gravity waves (IGWs) within a star can be fully converted to outward magnetic (MWs) if they encounter sufficiently strong field. The resulting dissipate as propagate regions with lower Alfv\'{e}n velocity. While tidal forcing is known excite IGWs, this conversion and subsequent damping of has not been explored dissipation mechanism. In particular, stars fields could tidally excited waves, yielding the same evolution previously-studied...

The details of the dynamo process that is responsible for driving solar magnetic activity cycle are still not fully understood. In particular, whilst differential rotation provides a plausible mechanism regeneration toroidal (azimuthal) component large-scale field, there ongoing debate regarding regenerating Sun's poloidal field. Our aim to demonstrate buoyancy, in presence rotation, capable producing necessary regenerative effect. Building upon our previous work, we carry out numerical...

The leading theoretical paradigm for the Sun's magnetic cycle is an $αω$-dynamo process, in which a combination of differential rotation and turbulent, helical flows produces large-scale field that reverses every 11 years. Most $αω$ solar dynamo models rely on tachocline to generate strong toroidal field. most problematic part such then production poloidal field, via process known as $α$-effect. Whilst this usually attributed small-scale convective motions under influence rotation,...

Turbulent convection is thought to act as an effective viscosity (νE) in damping tidal flows stars and giant planets. However, the efficiency of this mechanism has long been debated, particularly regime fast tides, when frequency (ω) exceeds turnover dominant convective eddies (ωc). We present results hydrodynamical simulations study interaction between a small patch zone. These build upon our prior work by simulating more turbulent larger horizontal boxes, here we explore wider range...

Tidal interactions are important in driving spin and orbital evolution various astrophysical systems such as hot Jupiters, close bi-nary stars, planetary satellites. However, the fluid dynamical mechanisms responsible for tidal dissipation giant planets stars remain poorly understood. One key mechanism is interaction between flows turbulent convection which thought to act an eddy viscosity dampening large scale flow. Using hydrodynamical simulations we investigate of equilibrium tide a...