Solar magnetic field (${\mathbf{B}}_{\odot }$)

The solar magnetic field is generated and maintained by electrically conducting flows through solar dynamo action. It includes a large-scale approximately dipolar component near activity minimum and strong, intermittent fields in active regions and sunspots. Its organized polarity reversals define the magnetic solar cycle. Magnetic stresses modify the generating flows, so a saturated dynamo requires nonlinear feedback as well as magnetic induction.

A spatially extended pattern of magnetic concentrations near boundaries of supergranulation. Surface transport and convergence redistribute magnetic elements into this network; flux emergence, cancellation and diffusion also continually modify it. It is distinct from the much smaller-scale field pattern in individual intergranular lanes and from the organized strong fields of sunspots.

The solar dynamo is the induction and regeneration of the solar magnetic field by conducting flows powered ultimately by solar convection and rotation. In a mean-field dynamo, differential rotation supplies the Omega effect and helical correlations or the Babcock-Leighton mechanism regenerate a poloidal magnetic field. The mean induction equation iswhere $\mathcal{E}=⟨\mathbf{u}\times \mathbf{b}⟩$ is the mean-field electromotive force. A model must close this correlation and include feedback to predict a saturated magnetic cycle; prescribing a shear alone does not close the regeneration loop.

Rotation influences convection, its helicity and differential rotation, which feed dynamo action. The generated magnetic field produces surface activity and strengthens the angular-momentum lever arm of a stellar wind. Wind braking lowers the rotation rate and ordinarily reduces unsaturated activity. Lorentz force feedback also changes the differential rotation and convective motions, saturating the dynamo on shorter time scales. Secular evolution, cyclic polarity reversal and irregular modulation are distinct time scales of this coupled system.

An interface solar dynamo separates the region of strong differential rotation from the region of poloidal-field regeneration, often placing shear near the tachocline and an alpha effect in the convection zone. Magnetic transport across the interface couples the two regions. The separation can provide toroidal-flux storage in a relatively stable layer, but growth, period and migration depend on the transport, diffusivity contrast, and signs of the regeneration and shear coefficients.

An ideal planar alpha-Omega dynamo places poloidal regeneration above an interface and shear-generated toroidal induction below it. With equal constant diffusivities, decay away from the interface and ordinary electromagnetic matching, its surface-wave branch grows when $D>32$ for positive $k,\alpha ,V$. The model separates the two regeneration regions while allowing diffusive coupling. The threshold refers to this model, not every solar interface dynamo or a full isotropic alpha closure.

Let $p=s-i\omega$ and $q^2=k^2+p/\eta$, with $\mathrm{Re}q>0$. The upper poloidal amplitude is $(A_0+Cz)e^{-qz}$ and the lower toroidal amplitude is $(B_0+cz)e^{qz}$. Their forcing equations give $2\eta qC=\alpha B_0$ and $-2\eta qc=ikV{A}_0$; interface matching gives $C=2q{A}_0$ and $c=-2q{B}_0$. Eliminating amplitudes yields the dispersion relation. Its potentially growing branch has $s=\eta k^2(\sqrt{D/32}-1)$ and $\omega =-\eta k^2\sqrt{D/32}$ with the convention $e^{ikx-i\omega t}$. The opposite branch decays.

For a planar interface, equal permeability and no singular sheet current make all magnetic components continuous. A nonzero horizontal Fourier wavenumber then gives the first three conditions in the title. Continuity of the tangential electric field supplies the last: continuous mean velocity cancels its advective contribution, and the retained alpha mean-field electromotive force is along the toroidal direction, so the other tangential electric component is $-U{\partial }_{x}A-\eta {\partial }_{z}B$. The given alpha-Omega equations retain only toroidal-to-poloidal alpha generation; adding a full isotropic alpha contribution would alter both the bulk equation and the matching problem.

A flux-transport solar dynamo couples toroidal and poloidal field generation through meridional advection, turbulent magnetic diffusion and possibly turbulent pumping. A common model uses the surface Babcock-Leighton mechanism, differential rotation near the tachocline, poleward surface circulation and an equatorward deep return flow. If advection dominates, circulation strongly influences the cycle period and migration; if diffusion dominates, diffusive coupling is important instead. Agreement with a butterfly pattern depends on the assumed transport geometry and coefficients, not merely on including a circulation term.

The Babcock-Leighton mechanism regenerates large-scale poloidal solar flux through the emergence and dispersal of systematically tilted bipolar active regions. With Joy's law tilt, opposite polarities have different latitudes: cancellation near the equator and poleward transport of surviving following-polarity flux alter and reverse the polar field. Thus a toroidal field that produces rising bipolar regions feeds back into a poloidal magnetic field. The source is intrinsically nonlocal between the interior flux reservoir and surface emergence and is stochastic because active-region fluxes and tilts vary.

A sunspot is a relatively cool, dark photospheric region associated with concentrated magnetic flux. The strong magnetic field inhibits convective heat transport, reducing the emergent local intensity. Spots commonly emerge in bipolar active regions, whose polarity and systematic tilt follow Hale's polarity law and Joy's law. Their number and latitude distribution are visible tracers of the solar cycle.

The axis of a bipolar solar active region is statistically tilted relative to the local east-west direction, with its following polarity typically farther from the equator and a mean tilt that grows with latitude. Scatter is substantial. The separation in latitude of the two polarities allows their surface dispersal to generate a net poloidal field through the Babcock-Leighton mechanism.

The solar cycle is the recurrent variation of magnetic activity, with a characteristic sunspot-number period of about eleven years. The large-scale magnetic polarity reverses from one activity cycle to the next, giving an approximately twenty-two-year magnetic cycle. Activity cycles vary in length and amplitude. A satisfactory solar dynamo model must account for polarity reversal, equatorward activity-belt migration in the solar butterfly diagram, the phase relation between polar and active-region fields, and long-term modulation including solar grand minima.

A solar grand minimum is a prolonged interval, lasting several ordinary cycles, of strongly reduced sunspot activity. Historical records identify the Maunder minimum; cosmogenic carbon-14 and beryllium-10 provide longer indirect records because stronger heliospheric magnetic shielding generally reduces cosmic-ray production of these isotopes. Weak activity does not imply a zero solar magnetic field. Proposed causes include stochastic weakening of poloidal-field generation, nonlinear dynamo modulation, and intermittency near an excitation threshold.

The Maunder minimum is the interval approximately 1645–1715 when recorded sunspot activity was exceptionally low. It is the best-known historical solar grand minimum. Historical coverage and cosmogenic-isotope records require care in inferring its precise magnetic amplitude; evidence for weak modulation need not imply that the normal spot-producing dynamo disappeared completely.

Bipolar solar active regions preferentially have one leading magnetic polarity in a given hemisphere and cycle, the opposite leading polarity in the other hemisphere, and reversed assignments in the next cycle. These statistical polarity rules reveal the ordered toroidal component of the solar magnetic field. Individual active regions can violate the preferred pattern, so the law is a statistical regularity rather than an exact rule for every spot pair.

A solar butterfly diagram plots sunspot occurrence or magnetic flux against latitude and time. New-cycle sunspot belts appear at middle latitudes and migrate toward the equator, producing successive wing-shaped patterns. Magnetic butterfly diagrams additionally show poleward flux transport and polar-field reversals. The diagram constrains both Parker dynamo wave propagation and magnetic transport in flux-transport solar dynamos.