Alfvén's theorem explained

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.

History

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]

Overview

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]

Flux tubes and field lines

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]

Mathematical statement

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,

where is the advective derivative.

Flux conservation

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

\iintB(t+\deltat)dS2-
\iint
S1
B(t)dS1
S2
\deltat

.

The surface integral over can be re expressed by applying Gauss's law for magnetism to assume that the magnetic flux through a closed surface formed by,, and the surface that connects the boundaries of and is zero. At time, this relationship can be expressed as

0=

-\iint
S1

B(t+\deltat)dS1+

\iint
S2

B(t+\deltat)dS2+

\iint
S3

B(t+\deltat)dS3,

where the sense of was reversed so that points outwards from the enclosed volume. In the surface integral over, the differential surface element where is the line element around the boundary of the surface . Solving for the surface integral over then gives
\iint
S2

B(t+\deltat)dS2=

\iint
S1

B(t+\deltat)dS1-

\oint
\partialS1

\left(v\deltat x B(t)\right)dl,

where the final term was rewritten using the properties of scalar triple products and a first-order approximation was taken. Substituting this into the expression for and simplifying results in
\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}

Applying the definition of a partial derivative to the integrand of the first term, applying Stokes' theorem to the second term, and combining the resultant surface integrals gives
D\PhiB
Dt

=

\iint
S1

\left(

\partialB
\partialt

-\nabla x \left(v x B\right)\right)dS1.

Using the ideal induction equation, the integrand vanishes, and
D\PhiB
Dt

=0.

Field line conservation

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(\nablav).

Using the mass continuity equation,
\partial\rho
\partialt

+(v\nabla)\rho=-\rho\nablav,

the ideal induction equation can be further rearranged to give
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

,which has the same form as the equation obtained previously for . Therefore, if and are initially parallel, they will remain parallel.

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,

whereas, for flux to be conserved, the fluid must satisfy the stronger condition imposed by the ideal induction equation.[8]

Kelvin's circulation theorem

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
} = \nabla \times (\mathbf\times\boldsymbol).However, the induction equation is linear, whereas there is a nonlinear relationship between and in the vorticity equation.[9]

Implications

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]

Resistive fluids

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})\nabla2\bf{B}+\nabla x (\bf{v} x \bf{B}),

in which, instead of fluid velocity, the flux velocity has been used. Although, in some cases, this velocity field can be found using magnetohydrodynamic equations, the existence and uniqueness of this vector field depends on the underlying conditions.[11]

Stochastic Alfvén theorem

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{}d{\bf{W}}(t)

in which is magnetic diffusivity and is the three-dimensional Gaussian white noise (see also Wiener process.) The many virtual field-vectors that arrive at the same final point must be averaged to obtain the physical magnetic field at that point.[14]

See also

Notes and References

  1. Alfvén. Hannes. On the Existence of Electromagnetic-Hydrodynamic Waves. Arkiv för matematik, astronomi och fysik. 1943. 29B(2). 1–7.
  2. Alfvén. Hannes. Existence of Electromagnetic-Hydrodynamic Waves. Nature. 1942. 150. 3805. 405. 10.1038/150405d0. 1942Natur.150..405A. 4072220.
  3. Alfvén . H. . August 1976 . On frozen-in field lines and field-line reconnection . Journal of Geophysical Research . en . 81 . 22 . 4019–4021 . 10.1029/JA081i022p04019. 1976JGR....81.4019A .
  4. Book: Priest . E. . Magnetic Reconnection . MHD Structures in Three-Dimensional Reconnection . Astrophysics and Space Science Library . 2016 . 427 . 101–142 . 10.1007/978-3-319-26432-5_3. 978-3-319-26430-1 .
  5. Book: Eric . Priest . Terry . Forbes . Magnetic Reconnection: MHD Theory and Applications . Cambridge University Press . First . 2000 . 0-521-48179-1 .
  6. Blackman . Eric G . On deriving flux freezing in magnetohydrodynamics by direct differentiation . European Journal of Physics . 1 March 2013 . 34 . 2 . 489–494 . 10.1088/0143-0807/34/2/489 . 1301.3562 . 2013EJPh...34..489B . 119247916 .
  7. Book: Lyu . Ling-Hsiao . Elementary Space Plasma Physics . 2010 . Airiti Press Inc . Taipei . 978-9868270954 . 173–176 . 12 January 2023.
  8. Eyink . Gregory L. . Aluie . Hussein . The breakdown of Alfvén's theorem in ideal plasma flows: Necessary conditions and physical conjectures . Physica D: Nonlinear Phenomena . November 2006 . 223 . 1 . 82–92 . 10.1016/j.physd.2006.08.009 . physics/0607073 . 2006PhyD..223...82E . 16529234 .
  9. Book: Gubbins . David . Herrero-Bervera . Emilio . Encyclopedia of Geomagnetism and Paleomagnetism . 2007 . Springer . Dordrecht . 978-1-4020-3992-8 . 7–11 . 10.1007/978-1-4020-4423-6 .
  10. Eyink. Gregory. Aluie. Hussein. The breakdown of Alfvén's theorem in ideal plasma flows: Necessary conditions and physical conjectures. Physica D: Nonlinear Phenomena. 2006. 223. 1. 82. 10.1016/j.physd.2006.08.009. physics/0607073. 2006PhyD..223...82E. 16529234.
  11. Wilmot-Smith. A. L.. Priest. E. R.. Horing. G.. Magnetic diffusion and the motion of field lines. Geophysical & Astrophysical Fluid Dynamics. 2005. 99. 2. 177–197. 10.1080/03091920500044808. 2005GApFD..99..177W. 51997635.
  12. Eyink. Gregory. Stochastic flux freezing and magnetic dynamo. Physical Review E. 2011. 83. 5. 056405. 10.1103/PhysRevE.83.056405. 21728673. 1008.4959. 2011PhRvE..83e6405E.
  13. Eyink. Gregory. Stochastic line motion and stochastic flux conservation for nonideal hydromagnetic models. Journal of Mathematical Physics. 2009. 50. 8. 083102. 10.1063/1.3193681. 0812.0153.
  14. Lalescu. Cristian C.. Shi. Yi-Kang. Eyink. Gregory. Drivas. Theodore D.. Vishniac. Ethan. Alexandre Lazarian. Lazarian. Alex. Inertial-Range Reconnection in Magnetohydrodynamic Turbulence and in the Solar Wind. Physical Review Letters. 2015. 115. 2. 025001. 10.1103/PhysRevLett.115.025001. 26207472. 1503.00509. 2015PhRvL.115b5001L. free.