In ideal magnetohydrodynamics, Alfvén's theorem, or the frozen-in flux theorem, states that electrically conducting fluids and embedded magnetic fields are constrained to move together in the limit of large magnetic Reynolds numbers. It is named after Hannes Alfvén, who put the idea forward in 1943.
Alfvén's theorem implies that the magnetic topology of a fluid in the limit of a large magnetic Reynolds number cannot change. This approximation breaks down in current sheets, where magnetic reconnection can occur.
The concept of magnetic fields being frozen into fluids with infinite electrical conductivity was first proposed by Hannes Alfvén in a 1943 paper titled "On the Existence of Electromagnetic-Hydrodynamic Waves", published in the journal Arkiv för matematik, astronomi och fysik. He wrote:[1] "On the Existence of Electromagnetic-Hydrodynamic Waves" interpreted the results of Alfvén's earlier paper "Existence of Electromagnetic-Hydrodynamic Waves", published in the journal Nature in 1942.[2]
Later in life, Alfvén advised against the use of his own theorem.[3]
Informally, Alfvén's theorem refers to the fundamental result in ideal magnetohydrodynamic theory that electrically conducting fluids and the magnetic fields within are constrained to move together in the limit of large magnetic Reynolds numbers (Rm)—such as when the fluid is a perfect conductor or when velocity and length scales are infinitely large. Motions of the two are constrained in that all bulk fluid motions perpendicular to the magnetic field result in matching perpendicular motion of the field at the same velocity and vice versa.
Formally, the connection between the movement of the fluid and the movement of the magnetic field is detailed in two primary results, often referred to as magnetic flux conservation and magnetic field line conservation. Magnetic flux conservation implies that the magnetic flux through a surface moving with the bulk fluid velocity is constant, and magnetic field line conservation implies that, if two fluid elements are connected by a magnetic field line, they will always be.[4]
Alfvén's theorem is frequently expressed in terms of magnetic flux tubes and magnetic field lines.
A magnetic flux tube is a tube- or cylinder-like region of space containing a magnetic field such that its sides are everywhere parallel to the field. Consequently, the magnetic flux through these sides is zero, and the cross-sections along the tube's length have constant, equal magnetic flux. In the limit of a large magnetic Reynolds number, Alfvén's theorem requires that these surfaces of constant flux move with the fluid that they are embedded in. As such, magnetic flux tubes are frozen into the fluid.
The intersection of the sides of two magnetic flux tubes form a magnetic field line, a curve that is everywhere parallel to the magnetic field. In fluids where flux tubes are frozen-in, it then follows that magnetic field lines must also be frozen-in. However, the conditions for frozen-in field lines are weaker than the conditions for frozen-in flux tubes, or, equivalently, for conservation of flux.[5]
In mathematical terms, Alfvén's theorem states that, in an electrically conducting fluid in the limit of a large magnetic Reynolds number, the magnetic flux through an orientable, open material surface advected by a macroscopic, space- and time-dependent velocity field is constant, or
| D\PhiB | |
| Dt |
=0,
In ideal magnetohydrodynamics, magnetic induction dominates over magnetic diffusion at the velocity and length scales being studied. The diffusion term in the governing induction equation is then assumed to be small relative to the induction term and is neglected. The induction equation then reduces to its ideal form:
| \partialB | |
| \partialt |
=\nabla x \left(v x B\right).
The conservation of magnetic flux through material surfaces embedded in the fluid follows directly from the ideal induction equation and the assumption of no magnetic monopoles through Gauss's law for magnetism.[6] [7]
In an electrically conducting fluid with a space- and time-dependent magnetic field and velocity field, an arbitrary, orientable, open surface at time is advected by in a small time to the surface . The rate of change of the magnetic flux through the surface as it is advected from to is then
| D\PhiB | |
| Dt |
=\lim\delta
| |||||||||||
| \deltat |
.
0=
| -\iint | |
| S1 |
B(t+\deltat) ⋅ dS1+
| \iint | |
| S2 |
B(t+\deltat) ⋅ dS2+
| \iint | |
| S3 |
B(t+\deltat) ⋅ dS3,
| \iint | |
| S2 |
B(t+\deltat) ⋅ dS2=
| \iint | |
| S1 |
B(t+\deltat) ⋅ dS1-
| \oint | |
| \partialS1 |
\left(v \deltat x B(t)\right) ⋅ dl,
| \begin{align} | D\PhiB |
| Dt |
=\lim\delta
| \iint | |
| S1 |
| B(t+\deltat)-B(t) | |
| \deltat |
⋅ dS1-
| \oint | |
| \partialS1 |
\left(v x B(t)\right) ⋅ dl. \end{align}
| D\PhiB | |
| Dt |
=
| \iint | |
| S1 |
\left(
| \partialB | |
| \partialt |
-\nabla x \left(v x B\right)\right) ⋅ dS1.
| D\PhiB | |
| Dt |
=0.
Field line conservation can also be derived mathematically using the ideal induction equation, Gauss's law for magnetism, and the mass continuity equation.
The ideal induction equation can be rewritten using a vector identity and Gauss's law for magnetism as
| \partialB | |
| \partialt |
=(B ⋅ \nabla)v-(v ⋅ \nabla)B-B(\nabla ⋅ v).
| \partial\rho | |
| \partialt |
+(v ⋅ \nabla)\rho=-\rho\nabla ⋅ v,
| D | \left( | |
| Dt |
| B | |
| \rho |
\right)=\left(
| B | |
| \rho |
⋅ \nabla\right)v.
Similarly, for a line segment where is the bulk plasma velocity at one end and is the velocity at the other end, the differential velocity between the two ends is and
| D\deltal | |
| Dt |
=(\deltal ⋅ \nabla)v
While flux conservation implies field line conservation (see), the conditions for the latter are weaker than the conditions for the former. Unlike the conditions for flux conservation, the conditions for field line conservation can be satisfied when an additional, source term parallel to the magnetic field is present in the ideal induction equation.
Mathematically, for field lines to be frozen-in, the fluid must satisfy
\left(
| \partialB | |
| \partialt |
-\nabla x \left(v x B\right)\right) x B=0,
Kelvin's circulation theorem states that vortex tubes moving with an ideal fluid are frozen to the fluid, analogous to how magnetic flux tubes moving with a perfectly conducting ideal-MHD fluid are frozen to the fluid. The ideal induction equation takes the same form as the equation for vorticity in an ideal fluid where is the velocity field:
| \partial\boldsymbol{\omega | |
Alfvén's theorem indicates that the magnetic field topology cannot change in a perfectly conducting fluid. However, in the case of complicated or turbulent flows, this would lead to highly tangled magnetic fields with very complicated topologies that should impede the fluid motions. Astrophysical plasmas with high electrical conductivities do not generally show such complicated tangled fields. Magnetic reconnection seems to occur in these plasmas unlike what would be expected from the flux freezing conditions. This has important implications for magnetic dynamos. In fact, a very high electrical conductivity translates into high magnetic Reynolds numbers, which indicates that the plasma will be turbulent.[10]
Even for the non-ideal case, in which the electric conductivity is not infinite, a similar result can be obtained by defining the magnetic flux transporting velocity by writing:
\nabla x (\bf{w} x \bf{B})=η\nabla2\bf{B}+\nabla x (\bf{v} x \bf{B}),
Research in the 21st century has claimed that the classical Alfvén theorem is inconsistent with the phenomenon of spontaneous stochasticity. Stochastic conservation laws developed to describe hydrodynamic behavior are shown to apply in the magnetohydrodynamic regime as well. Using the same tools produces results equivalent to that of classical Alfvén's theorem under ideal conditions, while also describing flux conservation and magnetic reconnection under non-ideal (real-world) conditions. Thus stochastic flux-freezing solutions can provide better descriptions of observed phenomena without relying on idealized conditions that are rare or even absent in the observed environment.[12] [13]
This generalized theorem states that magnetic field lines of the fine-grained magnetic field are "frozen-in" to the stochastic trajectories solving the following stochastic differential equation, known as the Langevin equation:
d{\bf{x}}={\bf{u}}({\bf{x}},t)dt+\sqrt{2η}d{\bf{W}}(t)