The magnetic field in the Sun's corona is often approximated as a force-free field.

A force-free magnetic field is a magnetic field in which the Lorentz force is equal to zero and the magnetic pressure greatly exceeds the plasma pressure such that non-magnetic forces can be neglected. For a force-free field, the electric current density is either zero or parallel to the magnetic field.

Definition

When a magnetic field is approximated as force-free, all non-magnetic forces are neglected and the Lorentz force vanishes. For non-magnetic forces to be neglected, it is assumed that the ratio of the plasma pressure to the magnetic pressure—the plasma β—is much less than one, i.e., . With this assumption, magnetic pressure dominates over plasma pressure such that the latter can be ignored. It is also assumed that the magnetic pressure dominates over other non-magnetic forces, such as gravity, so that these forces can similarly be ignored.

In SI units, the Lorentz force condition for a static magnetic field can be expressed as

where

is the current density and is the vacuum permeability. Alternatively, this can be written as

These conditions are fulfilled when the current vanishes or is parallel to the magnetic field.[1]

Zero current density

If the current density is identically zero, then the magnetic field is the gradient of a magnetic scalar potential :

The substitution of this into results in Laplace's equation, which can often be readily solved, depending on the precise boundary conditions. In this case, the field is referred to as a potential field or vacuum magnetic field.

Nonzero current density

If the current density is not zero, then it must be parallel to the magnetic field, i.e., where is a scalar function known as the force-free parameter or force-free function. This implies that

The force-free parameter can be a function of position but must be constant along field lines.

Linear force-free field

When the force-free parameter is constant everywhere, the field is called a linear force-free field (LFFF). A constant allows for the derivation of a vector Helmholtz equation

by taking the curl of the nonzero current density equations above.

Nonlinear force-free field

When the force-free parameter depends on position, the field is called a nonlinear force-free field (NLFFF). In this case, the equations do not possess a general solution, and usually must be solved numerically.[1][2][3]: 50–54 

Physical examples

In the Sun's upper chromosphere and lower corona, the plasma β can locally be of order 0.01 or lower allowing for the magnetic field to be approximated as force-free.[1][4][5][6]

See also

References

  1. 1 2 3 Wiegelmann, Thomas; Sakurai, Takashi (December 2021). "Solar force-free magnetic fields" (PDF). Living Reviews in Solar Physics. 18 (1): 1. doi:10.1007/s41116-020-00027-4. S2CID 232107294. Retrieved 18 May 2022.
  2. ↑ Bellan, Paul Murray (2006). Fundamentals of plasma physics. Cambridge: Cambridge University Press. ISBN 0521528003.
  3. ↑ Parker, E. N. (2019). Cosmical Magnetic Fields: Their Origin and Their Activity. Oxford: Clarendon Press. ISBN 978-0-19-882996-6.
  4. ↑ Amari, T.; Aly, J. J.; Luciani, J. F.; Boulmezaoud, T. Z.; Mikic, Z. (1997). "Reconstructing the Solar Coronal Magnetic Field as a Force-Free Magnetic Field". Solar Physics. 174: 129–149. Bibcode:1997SoPh..174..129A. doi:10.1023/A:1004966830232.
  5. ↑ Low, B. C.; Lou, Y. Q. (March 1990). "Modeling Solar Force-Free Magnetic Fields". The Astrophysical Journal. 352: 343. Bibcode:1990ApJ...352..343L. doi:10.1086/168541.
  6. ↑ Peter, H.; Warnecke, J.; Chitta, L. P.; Cameron, R. H. (November 2015). "Limitations of Force-Free Magnetic Field Extrapolations: Revisiting Basic Assumptions". Astronomy & Astrophysics. 584. arXiv:1510.04642. Bibcode:2015A&A...584A..68P. doi:10.1051/0004-6361/201527057.
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.