Inevitability of a magnetic field in the Sun's radiative interior

  title={Inevitability of a magnetic field in the Sun's radiative interior},
  author={D. Gough and M. McIntyre},
The gas in the convective outer layers of the Sun rotates faster at the equator than in the polar regions, yet deeper inside (in the radiative zone) the gas rotates almost uniformly. There is a thin transition layer between these zones, called the tachocline. This structure has been measured seismologically, but no purely fluid-dynamical mechanism can explain its existence. Here we argue that a self-consistent model requires a large-scale magnetic field in the Sun's interior, as well as… Expand
Propagation of a dynamo field in the radiative interior of the Sun
ABSTRA C T Large-scale magnetic fields are believed to play an important role in the radiative zone of the Sun, in particular in the dynamical processes in the transition region between theExpand
We present axisymmetric simulations of the coupled convective and radiative regions in the Sun in order to investigate the angular momentum evolution of the radiative interior. Both hydrodynamic andExpand
To date, no self-consistent numerical simulation of the solar interior has succeeded in reproducing the observed thinness of the solar tachocline and the persistence of uniform rotation beneath it.Expand
Magnetic confinement of the solar tachocline
Context. We study the physics of the solar tachocline (i.e. the thin transition layer between differential rotation in the convection zone and quasi uniform rotation in the radiative interior), andExpand
Turbulent dynamo near tachocline and reconstruction of azimuthal magnetic field in the solar convection zone
In order to extend the abilities of the αΩ dynamo model to explain the observed regularities and anomalies of the solar magnetic activity, the negative buoyancy phenomenon and the magnetic quenchingExpand
Polar confinement of the Sun's interior magnetic field by laminar magnetostrophic flow
The global-scale interior magnetic field Bi needed to account for the Sun's observed differential rotation can be effective only if confined below the convection zone in all latitudes including, mostExpand
The global dynamics of a rotating star like the Sun involves the coupling of a highly turbulent convective envelope overlying a seemingly benign radiative interior. We use the anelastic sphericalExpand
On the Penetration of Meridional Circulation Below the Solar Convection Zone. II. Models with Convection Zone, the Taylor-Proudman Constraint, and Applications to Other Stars
The solar convection zone exhibits a strong level of differential rotation, whereby the rotation period of the polar regions is about 25%-30% longer than the equatorial regions. The Coriolis forceExpand
Magnetic confinement of the solar tachocline: II. Coupling to a convection zone
Context. The reason for the observed thinness of the solar tachocline is still not well understood. One of the explanations that have been proposed is that a primordial magnetic field renders theExpand
Dynamo action in simulations of penetrative solar convection with an imposed tachocline
We summarize new and continuing three-dimensional spherical shell simulations of dynamo action by convection allowed to penetrate downward into a tachocline of rotational shear. The inclusion of anExpand


Aspects of the solar tachocline
The splitting of the frequencies of p-mode multiplets enables information to be gained about the internal rotation of the sun. Such data have revealed a transition at the base of the convection zoneExpand
Angular momentum transport by internal waves in the solar interior
The internal gravity waves of low frequency which are emitted at the base of the solar convection zone are able to extract angular momentum from the radiative interior. We evaluate this transportExpand
Angular momentum transport by gravity waves and its effect on the rotation of the solar interior
We calculate the excitation of low-frequency gravity waves by turbulent convection in the Sun and the effect of the angular momentum carried by these waves on the rotation profile of the Sun'sExpand
The Seismic Structure of the Sun
Global Oscillation Network Group data reveal that the internal structure of the sun can be well represented by a calibrated standard model. However, immediately beneath the convection zone and at theExpand
On the “Downward Control” of Extratropical Diabatic Circulations by Eddy-Induced Mean Zonal Forces
Abstract The situation considered is that of a zonally symmetric model of the middle atmosphere subject to a given quasi-steady zonal force F, conceived to be the result of irreversible angularExpand
Differential Rotation and Dynamics of the Solar Interior
Frequency splittings derived from GONG observations confirm that the variation of rotation rate with latitude seen at the surface carries through much of the convection zone, at the base of which is an adjustment layer leading to latitudinally independent rotation at greater depths. Expand
Calibration of the Thickness of the Solar Tachocline
Material circulation in the solar tachocline mixes the tachocline material with the convection zone, which causes the sound speed in and immediately beneath the tachocline to exceed what one wouldExpand
On possible origins of relatively short-term variations in the solar structure
  • D. Gough
  • Environmental Science, Physics
  • Philosophical Transactions of the Royal Society of London. Series A, Mathematical and Physical Sciences
  • 1990
The general large-scale redistribution of magnetic field over the solar cycle is possibly associated with an overall variation of thermal structure of the convection zone, which modulates not onlyExpand
The Instability of a Forced Standing Wave in a Viscous Stratified Fluid: A Laboratory Analogue of .the Quasi-Biennial Oscillation
Abstract An experiment is described in which a standing internal wave is forced at the lower boundary of an annulus of salt-stratified water. At sufficiently large forcing amplitudes, the wave motionExpand
The Maunder Minimum and the Solar Dynamo
On the basis of systematic observations of sunspots available since Galilei’s time, we have been able to derive certain properties of normal and low-activity cycles, such as those of the MaunderExpand