- Research Letter
- Open Access
Comparison of current disruption and magnetic reconnection
© Lui. 2015
Received: 14 October 2015
Accepted: 17 November 2015
Published: 1 December 2015
We examine similarities and differences between the concepts of current disruption (CD) and magnetic reconnection (MR). Both concepts have been invoked to account for explosive phenomena that involve energy transformation from magnetic field to charged particles. Similarities of these two concepts include (1) the occurrence of breakdown in magnetic connectivity, (2) magnetic energy as the primary energy source, and (3) plasma energization as a product of the process. Differences include (1) plasma flow across separatrix surfaces in an X-type magnetic field geometry being essential for MR but not for CD, (2) plasma flow ordered by the magnetic field geometry for MR but not for CD, (3) field line topology change essential for MR but not necessary for CD, and (4) CD exhibiting multifractal and symmetry breaking behavior while no such behavior has been investigated for MR. Overall, CD can be viewed as a form of generalized MR (GMR) in which the requirement for a specific magnetic field geometry and its constraint on the plasma flow pattern are removed. Therefore, the CD concept has a broader scope in applications than the MR concept alone.
Identifying physical processes responsible for impulsive release of energy in the magnetosphere, and more generally in space plasmas, is an outstanding unsolved problem. These energetic processes call for the breakdown of the frozen-in-field condition such that magnetic energy can be transformed to charged particle energy. Magnetic reconnection (MR) is the most favorite mechanism invoked to account for many observed impulse energetic phenomena in the space and astrophysics communities. The concept of MR appeared first in the solar physics community, introduced by Giovanelli (1946) in an attempt to explain particle acceleration in solar flares. He suggested that flare emissions could be due to electrons accelerated by inductive electric fields near neutral points in the evolving magnetic fields of sunspots. This original concept was developed further by Sweet (1958), Parker (1957), Dungey (1961) and Petschek (1964).
The early concept of MR was relatively simple and developed for a two-dimensional (2D) geometry under relatively steady-state condition. In this situation, MR can be defined as the process whereby plasma flows across a surface that separates regions containing topologically different magnetic field lines. Such a separatrix surface (or line in projection) exists in a 2D configuration, where different branches of magnetic field lines join in an X-type neutral line (point) or, more generally, in Y-lines (points).
The central grey region is called the ion diffusion region. Inside the ion diffusion region, the motion of ions departs from that of electrons and magnetic field line motion is ill defined. This situation is often referred to as the breakdown of the frozen-in-field condition. The ions are accelerated by the Lorentz force at the separatrix surfaces, indicated by dash-lines in Fig. 1, and are ejected out on the two sides of the ion diffusion region as depicted by the red arrows in Fig. 1. The electrons still do the E y × B drift until they reach the electron diffusion region deep inside the ion diffusion region. The differential motion of ions and electrons in the ion diffusion region creates an electric current and an electric field E z inside the ion diffusion region. The current and electric field generated this way are oppositely directed and form a dynamo that drives currents in the vicinity of the separatrix surfaces. This current system produces the quadruple pattern of magnetic perturbations pointing perpendicular to the 2D reconnection plane, as shown in Fig. 1 by the sign of B y.
Inside the electron diffusion region, electrons are no longer confined to E y × B drift and can move along the X-line. They gain energy from the electric field E y in the process and eventually move out of this region.
The key outstanding problem in MR is to understand what physical processes are needed to break the frozen-in-field condition in both the ion and electron diffusion regions.
Since nature is three-dimensional (3D), the depiction of MR in a 2D plane as indicated by Fig. 1 is deficient. In addition, impulsive energy release phenomena are highly transient and cannot be represented by a relatively steady-state situation. As a result, there were efforts to broaden the 2D nature of the MR concept. For example, Schindler et al. (1988) proposed generalized magnetic reconnection (GMR) to represent processes by which a breakdown of magnetic connection occurs due to a localized non-idealness in magnetohydrodynamics (MHD) formalism. However, this definition is deemed too broad-brush because it includes all non-MHD processes that are not intended for MR originally. As an example of this deficiency, the non-idealness caused by the presence of an electric field E || along the magnetic field line above an auroral arc would be considered as GMR even though no magnetic field line could be visualized to be “cut” and “joined” with another magnetic field line. More importantly, the bulk acceleration resulting in the whole plasma population jetting out of a MR site is absent in this case.
Another effort to generalize 2D picture of MR to 3D situation was put forth by Lui et al. (2005) based on the outcome of a workshop held in Kiruna, Sweden on 2002 September 18–20 to discuss the extension of MR to 3D and to non-steady-state condition. They proposed that MR process has the following intrinsic characteristics: (1) there is a plasma bulk flow across a boundary separating regions with topologically different magnetic field lines if projected on the plane of MR; (2) there can be an out-of-the-plane magnetic field component (so-called guide field) present such that the reconnected magnetic flux tubes become twisted to form magnetic flux ropes; (3) the guide field cannot be stronger by an order of magnitude or more than the magnetic field in the plasma inflow region without the guide field component; (4) the region exhibiting non-ideal MHD condition should be localized to a scale comparable to the ion inertial length in the direction of the plasma inflow velocity.
The CD location was close to the Earth and the magnetic field there was strong even though its magnitude before CD was much reduced from the dipole value. The magnetic field characteristics was unlike that from the approximately one-dimensional (1D) current sheet in the magnetotail. The observed features are those expected for the transition region from dipolar field geometry to tail-like geometry.
Later analysis of a similar CD event showed the existence of multiple frequency components and intermittent intensification in the observed magnetic disturbances (Lui and Najmi 1997). The study indicates that CD is a multiscale process and has the intrinsic signatures of plasma turbulence. They surmised that CD leads to current sheet becoming filamentary, current pattern displaying complex distribution and topology. The interval may include embedded reversals in the current density direction. Furthermore, the associated plasma flow pattern in the turbulent medium is not ordered by the magnetic field pattern, unlike that in MR.
A study of CD involves understanding plasma turbulence. Consolini and Lui (1999, 2000) has applied tools in complex system dynamics to examine properties of CD. From an analysis of structure function on magnetic fluctuations to obtain the Holder exponent H, they noted that H is about 0.5 before CD onset, which is similar to Brownian motion. However, after CD, H is about 0.7, implying longer persistency of magnetic fluctuations and the appearance of a new ordered phase having a different symmetry, i.e., symmetry breaking by the occurrence of CD. In addition, they performed wavelet bicoherence analysis to show bursts of coherency indicative of intermittency in phase coupling and strong three-wave interaction. These activities can lead to inverse cascade, i.e., the decay moves from small scales to large scales, as observations indicated (Lui and Najmi 1997; Lui 2008). Further study of structure function shows the multifractal and intermittent nature of CD as well (Lui 2001). As CD involves plasma turbulence, it poses a challenging problem to solve since it is well recognized in the physics community at large that turbulence is an outstanding unsolved problem in classical physics (Falkovich and Sreenivasan 2006).
From the above studies, one may define CD as a process by which the current density reduces by a significant fraction of its value in a short time scale comparable to or shorter than the local ion gyroperiod. It has multiscale properties, characteristics of turbulence. The current reduction usually requires instability of the system.
Summary and discussion
Energy transformation from magnetic field to charged particles is a challenging topic in space and astrophysics communities. Both MR and CD have been invoked to explain impulsive release of energy in explosive phenomena observed in nature. The above review shows some similarities and differences between the concepts of CD and MR. Similarities include (1) the occurrence of breakdown in magnetic connectivity, (2) magnetic energy as the primary energy source for the process, and (3) plasma energization as a product of the process. Differences include (1) plasma flow across separatrix surfaces in an X-type magnetic field geometry regarded as essential for MR but not necessarily for CD, (2) plasma flow ordered by the magnetic field geometry for MR but not for CD, (3) field line topology change essential for MR but not necessarily for CD, and (4) CD exhibiting a multifractal and symmetry breaking behavior while no such behavior has been revealed for MR.
Overall, CD is more general than MR since it can release magnetic energy explosively without the requirement that magnetic topology has to be changed in the process. In this way, CD is a generalized form of MR. One advantage of adopting the CD concept is that no motion of magnetic field line is needed to describe the process. Since motion of magnetic field line is non-unique (Newcomb 1958; Vasyliunas 1972; Roth 2003), replacing MR by CD can eliminate the ill-defined, and unphysical in opinions of other branches of physics, notion of magnetic field line motion. Some pioneering scientists in the space community have emphasized the inapplicability of field line reconnection in discussions of auroral and magnetospheric theory (Alfvén 1976, 1977; Parks 2004; Akasofu 2013, 2015).
This work was supported by the NSF Grants AGS-1250634 and the NASA Grants NNX12AP62G to The Johns Hopkins University Applied Physics Laboratory.
The author declares that he has no competing interests.
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- Akasofu S-I. The development of the auroral substorm. Planet Space Sci. 1964;12:273–82.View ArticleGoogle Scholar
- Akasofu SI. Magnetospheric substorms: a model. In: Dyer ER, editor. Solar terrestrial physics, Part III. D. Reidel Publ. Co. 1972. pp. 131.Google Scholar
- Akasofu S-I. Where is the magnetic energy for the expansion phase of auroral substorms accumulated? J Geophys Res. 2013;118(1):7. doi:10.1002/2013JA019042.Google Scholar
- Akasofu S-I. Auroral substorms as an electrical discharge phenomenon. Prog Earth Planbetary Sci. 2015;2:20. doi:10.1186/s40645-015-0050-9.View ArticleGoogle Scholar
- Alfvén H. Existence of electromagnetic–hydrodynamic waves. Nature. 1942;150:405.View ArticleGoogle Scholar
- Alfvén H. On frozen-in field lines and field-line reconnection. J Geophys Res. 1976;81:4019–21.View ArticleGoogle Scholar
- Alfvén H. Electrical currents in cosmic plasmas. Rev Geophys. 1977;15:271–84.View ArticleGoogle Scholar
- Atkinson G. An approximate flow equation for geomagnetic flux tubes and its application to polar substorms. J Geophys Res. 1967;72:5373–82.View ArticleGoogle Scholar
- Consolini G, Lui ATY. Sign-singularity analysis of current disruption. Geophys Res Lett. 1999;26:1673.View ArticleGoogle Scholar
- Consolini G, Lui ATY. Symmetry breaking and nonlinear wave–wave interaction in current disruption: possible evidence for a dynamical phase transition. In: Ohtani SI, Fujii R, Hesse M, Lysak RL, AGU, editors. Magnetospheric current systems. AGU geophysical monograph 118. Washington, DC. 2000. pp. 395.Google Scholar
- Dungey JW. Interplanetary magnetic field and the auroral zones. Phys Res Lett. 1961;6:47–8.View ArticleGoogle Scholar
- Falkovich G, Sreenivasan K. Lessons from hydrodynamic turbulence. Phys Today. 2006;59(4):43–9. doi:10.1063/1.2207037.View ArticleGoogle Scholar
- Giovanelli RG. A theory of chromospheric flares. Nature. 1946;158:81.View ArticleGoogle Scholar
- Lui ATY, Lopez RE, Krimigis SM, McEntire RW, Zanetti LJ, Potemra TA. A case study of magnetotail current sheet disruption and diversion. Geophys Res Lett. 1988;15:721–4.View ArticleGoogle Scholar
- Lui ATY, Najmi A-H. Time–frequency decomposition of signals in a current disruption event. Geophys Res Lett. 1997;24:3157–60.View ArticleGoogle Scholar
- Lui ATY. Multifractal and intermittent nature of substorm-associated magnetic turbulence in the magnetotail. J Atmos Solar Terr Phys. 2001;63:1379–85.View ArticleGoogle Scholar
- Lui ATY, Jacquey C, Lakhina GS, Lundin R, Nagai T, Phan T-D, Pu ZY, Roth M, Song Y, Treumann RA, Yamauchi M, Zelenyi LM. Critical issues on magnetic reconnection in space plasmas. Space Sci Rev. 2005;116:497–521.View ArticleGoogle Scholar
- Lui ATY, Yoon PH, Mok C, Ryu CM. Inverse cascade feature in current disruption. J Geophys Res. 2008;113:A00C06. doi:10.1029/2008JA013521.Google Scholar
- Newcomb WA. Motion of magnetic lines of force. Ann Phys. 1958;3:347–85.View ArticleGoogle Scholar
- Parker EN. Sweet’s mechanism for merging magnetic fields in conducting fluids. J Geophys Res. 1957;62:509–20. doi:10.1029/JZ062i004p00509.View ArticleGoogle Scholar
- Parks GK. Why space physics need to go beyond the MHD box. Space Sci Rev. 2004;113:97–125.View ArticleGoogle Scholar
- Petschek HE. Magnetic field annihilation. AAS-NASA Symposium on the Physics of Solar Flares, NASA Spec. Publ. SP-50. 1964. pp. 425–439.Google Scholar
- Roth M. Magnetic reconnection and physical concepts, Proceedings of the Magnetic Reconnection Meeting, Kiurna, Sweden, September 2002. IRF Sci Rep. 2003;280:19–24.Google Scholar
- Schindler K, Hesse M, Birn J. Magnetic reconnection, parallel electric field, and helicity. J Geophys Res. 1988;93:5547–57.View ArticleGoogle Scholar
- Siscoe GL, Cummings WD. On the cause of geomagnetic bays. Planet Space Sci. 1969;17:1795–802.View ArticleGoogle Scholar
- Sweet, P. A. (1958), The neutral point theory of solar flares, Proceedings of the International Astronomical Union Symposium on Electromagnetic Phenomena in Cosmical Physics, No. 6 (Stockholm, 1956). pp. 123–134.Google Scholar
- Takahashi K, Zanetti LJ, Lopez RE, McEntire RW, Potemra TA, Yumoto K. Disruption of the magnetotail current sheet observed by AMPTE/CCE. Geophys Res Lett. 1987;14:1019–22.View ArticleGoogle Scholar
- Vasyliunas VM. Nonuniqueness of magnetic field line motion. J Geophys Res. 1972;77:6271–4.View ArticleGoogle Scholar