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| [[Image:reconnection.gif|right|thumb|380px|Magnetic Reconnection: This view is a cross-section through four magnetic domains undergoing separator reconnection. Two separatrices (see text) divide space into four magnetic domains with a separator at the center of the figure. Field lines (and associated plasma) flow inward from above and below the separator, reconnect, and spring outward horizontally. A current sheet (as shown) may be present but is not required for reconnection to occur. This process is not well understood: once started, it proceeds many orders of magnitude faster than predicted by standard models.]]
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| [[File:SDO Observes a Reconnection Event.ogg|thumb|380px|A magnetic reconnection event on the [[sun]].]]
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| '''Magnetic reconnection''' is a physical process in highly conducting [[Plasma (physics)|plasmas]] in which the magnetic [[topology]] is rearranged and magnetic energy is converted to [[kinetic energy]], [[thermal energy]], and [[particle acceleration]]. Magnetic reconnection occurs on timescales intermediate between slow resistive diffusion of the [[magnetic field]] and fast [[Alfvén wave|Alfvénic]] timescales.
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| The qualitative description of the reconnection process is such that magnetic field lines from different [[magnetic domain]]s (defined by the field line connectivity) are spliced to one another, changing their patterns of connectivity with respect to the sources. It is a violation of an approximate conservation law in plasma physics, and can concentrate mechanical or magnetic energy in both space and time. [[Solar flare]]s, the largest explosions in the [[Solar System]], may involve the reconnection of large systems of magnetic flux on the [[Sun]], releasing, in minutes, energy that has been stored in the magnetic field over a period of hours to days. Magnetic reconnection in [[Earth]]'s [[magnetosphere]] is one of the mechanisms responsible for the [[Aurora (astronomy)|aurora]], and it is important to the science of controlled [[nuclear fusion]] because it is one mechanism preventing [[magnetic confinement]] of the fusion fuel.
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| In an electrically conductive [[Plasma (physics)|plasma]], magnetic field lines are grouped into 'domains'— bundles of field lines that connect from a particular place to another particular place, and that are topologically distinct from other field lines nearby. This topology is approximately preserved even when the magnetic field itself is strongly distorted by the presence of variable currents or motion of magnetic sources, because effects that might otherwise change the magnetic topology instead induce [[eddy current]]s in the plasma; the eddy currents have the effect of canceling out the topological change.
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| In two dimensions, the most common type of magnetic reconnection is '''separator reconnection''', in which four separate magnetic domains exchange magnetic field lines. Domains in a magnetic plasma are separated by ''[[Separatrix (Math)|separatrix]] surfaces'': curved surfaces in space that divide different bundles of flux. Field lines on one side of the separatrix all terminate at a particular magnetic pole, while field lines on the other side all terminate at a different pole of similar sign. Since each field line generally begins at a north magnetic pole and ends at a south magnetic pole, the most general way of dividing simple flux systems involves four domains separated by two separatrices: one separatrix surface divides the flux into two bundles, each of which shares a south pole, and the other separatrix surface divides the flux into two bundles, each of which shares a north pole. The intersection of the separatrices forms a ''separator'', a single line that is at the boundary of the four separate domains. In separator reconnection, field lines enter the separator from two of the domains, and are spliced one to the other, exiting the separator in the other two domains (see the figure).
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| According to simple resistive [[magnetohydrodynamics]] (MHD) theory, reconnection happens because the plasma's [[resistivity|electrical resistivity]] near the boundary layer opposes the [[current (electricity)|current]]s necessary to sustain the change in the magnetic field. The need for such a current can be seen from one of [[Maxwell's equations]],
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| : <math>\nabla \times \mathbf{B} = \mu \mathbf{J} + \mu \epsilon \frac{\partial \mathbf{E}}{\partial t}.</math>
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| The resistivity of the current layer allows [[magnetic flux]] from either side to diffuse through the current layer, cancelling out flux from the other side of the boundary. When this happens, the plasma is pulled out by [[Magnetic tension force|magnetic tension]] along the direction of the magnetic field lines. The resulting drop in pressure pulls more plasma and magnetic flux into the central region, yielding a self-sustaining process.
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| A current problem in plasma [[physics]] is that observed reconnection happens much faster than predicted by MHD in high [[Lundquist number]] plasmas: solar flares, for example, proceed 13-14 orders of magnitude faster than a naive calculation would suggest, and several orders of magnitude faster than current theoretical models that include turbulence and kinetic effects. There are two competing theories to explain the discrepancy. One posits that the electromagnetic [[turbulence]] in the boundary layer is sufficiently strong to scatter electrons, raising the plasma's local resistivity. This would allow the magnetic flux to diffuse faster.
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| ==Theoretical descriptions of magnetic reconnection==
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| ===The Sweet-Parker Model===
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| At a conference in 1956, Peter Sweet pointed out that by pushing two plasmas with oppositely directed magnetic fields together, resistive diffusion is able to occur on a length scale much shorter than a typical equilibrium length scale.<ref>Sweet, P. A., The Neutral Point Theory of Solar Flares, in IAU Symposium 6, Electromagnetic Phenomena in Cosmical Physics, ed. B. Lehnert (Dordrecht: Kluwer), 123, 1958</ref> [[Eugene Parker]] was in attendance at this conference and developed scaling relations for this model during his return travel.<ref>Parker, E. N., Sweet's Mechanism for Merging Magnetic Fields in Conducting Fluids, J. Geophys. Res., 62, 509, 1957</ref>
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| The Sweet-Parker model describes time-independent magnetic reconnection in the resistive MHD framework when the reconnecting magnetic fields are antiparallel (oppositely directed) and effects related to viscosity and compressibility are unimportant. The ideal [[Ohm's law]] then yields the relation
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| : <math> E_y = V_{in} B_{in} </math> | |
| where <math>E_y</math> is the out-of-plane electric field, <math>V_{in}</math> is the characteristic inflow velocity, and <math>B_{in}</math> is the characteristic upstream magnetic field strength. By neglecting displacement current, the low-frequency Ampere's law, <math>\mathbf{J} = \frac{\nabla\times\mathbf{B}}{\mu_0}</math>, gives the relation
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| : <math> J_y \sim \frac{B_{in}}{\mu_0\delta}, </math>
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| where <math>\delta</math> is the current sheet half-thickness. This relation uses that the magnetic field reverses over a distance of <math>\sim2\delta</math>. By matching the ideal electric field outside of the layer with the resistive electric field, <math>\mathbf{E}=\eta\mathbf{J}</math>, inside the layer, we find that
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| : <math>V_{in} \sim \frac{\eta}{\mu_0\delta},</math>
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| where <math>\eta</math> is the plasma resistivity. When the inflow density is comparable to the outflow density, conservation of mass yields the relationship
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| : <math>V_{in}L \sim V_{out}\delta, </math>
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| where <math>L</math> is the half-length of the current sheet and <math>V_{out}</math> is the outflow velocity. The left and right hand sides of the above relation represent the mass flux into the layer and out of the layer, respectively. Equating the upstream magnetic pressure with the downstream [[dynamic pressure]] gives
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| : <math>\frac{B_{in}^2}{2\mu_0} \sim \frac{\rho V_{out}^2}{2} </math>
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| where <math>\rho</math> is the mass density of the plasma. Solving for the outflow velocity then gives
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| : <math> V_{out} \sim V_A \equiv \frac{B_{in}}{\sqrt{\mu_0 \rho}} </math>
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| where <math>V_A</math> is the [[Alfvén wave|Alfvén]] velocity. The dimensionless reconnection rate can then be written as
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| : <math> \frac{V_{in}}{V_A} \sim \frac{1}{S^{1/2}} </math>
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| where the dimensionless [[Lundquist number]] <math>S</math> is given by
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| : <math> S \equiv \frac{\mu_0 L V_A}{\eta}. </math>
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| Sweet-Parker reconnection allows for reconnection rates much faster than global diffusion, but is not able to explain the fast reconnection rates observed in solar flares, the Earth's magnetosphere, and laboratory plasmas. Additionally, Sweet-Parker reconnection neglects three-dimensional effects, collisionless physics, time-dependent effects, viscosity, compressibility, and downstream pressure. Numerical simulations of two-dimensional magnetic reconnection typically show agreement with this model.<ref>Biskamp, D., Magnetic reconnection via current sheets, Physics of Fluids, 29, 1520, 1986</ref> Results from the Magnetic Reconnection Experiment (MRX) of collisional reconnection show agreement with a generalized Sweet-Parker model which incorporates compressibility, downstream pressure, and anomalous resistivity.<ref>Ji, H., M. Yamada, S. Hsu, R. Kulsrud, T. Carter, & S. Zaharia, Magnetic reconnection with Sweet-Parker characteristics in two-dimensional laboratory plasmas, Physics of Plasmas, 6, 1743, 1999</ref>
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| ===Petschek reconnection=== | |
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| One of the reasons why Sweet-Parker reconnection is slow is that the aspect ratio of the reconnection layer is very large in high Lundquist number plasmas. The inflow velocity, and thus the reconnection rate, must then be very small. In 1964, Harry Petschek proposed a mechanism where the inflow and outflow regions are separated by stationary slow mode shocks.<ref>Petschek, H. E., Magnetic Field Annihilation, in The Physics of Solar Flares, Proceedings of the AAS-NASA Symposium held 28–30 October 1963 at the Goddard Space Flight Center, Greenbelt, MD, p. 425, 1964</ref> The aspect ratio of the diffusion region is then of order unity and the maximum reconnection rate becomes
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| : <math> \frac{V_{in}}{V_A} \approx \frac{\pi}{8 \ln S}. </math>
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| This expression allows fast reconnection almost independent of the Lundquist number.
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| Simulations of resistive MHD reconnection with uniform resistivity showed the development of elongated current sheets in agreement with the Sweet-Parker model rather than the Petschek model. When a localized anomalously large resistivity is used, however, Petschek reconnection can be realized in resistive MHD simulations. Because the use of an anomalous resistivity is only appropriate when the particle mean free path is large compared to the reconnection layer, it is likely that other collisionless effects become important before Petschek reconnection can be realized.
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| ===Collisionless reconnection===
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| On length scales shorter than the ion inertial length <math>c/\omega_{pi}</math> (where <math>\omega_{pi}\equiv \sqrt{\frac{n_iZ^2e^2}{\epsilon_0m_i}}</math> is the ion plasma frequency), [[ion]]s decouple from electrons and the magnetic field becomes frozen into the electron fluid rather than the bulk plasma. On these scales the [[Hall effect]] becomes important. Two-fluid simulations show the formation of an X-point geometry rather than the double Y-point geometry characteristic of resistive reconnection. The [[electron]]s are then accelerated to very high speeds by [[Electromagnetic electron wave|Whistler waves]]. Because the ions can move through a wider "bottleneck" near the current layer and because the electrons are moving much faster in Hall MHD than in [[Magnetohydrodynamics|standard MHD]], reconnection may proceed more quickly. Two-fluid/collisionless reconnection is particularly important in the Earth's magnetosphere.
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| ==Observations of magnetic reconnection in nature and the laboratory==
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| ===The Solar Atmosphere===
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| Magnetic reconnection occurs during [[solar flare]]s, [[coronal mass ejection]]s, and many other events in the solar atmosphere. The observational evidence for solar flares includes observations of inflows/outflows, downflowing loops, and changes in the magnetic topology. In the past observations of the solar atmosphere were done using remote imaging; consequently, the magnetic fields were inferred or extrapolated rather than observed directly. However, the first direct observations of solar magnetic reconnection were gathered in 2012 (and released in 2013) by the [[High Resolution Coronal Imager]].<ref>{{cite web|url=http://www.azonano.com/news.aspx?newsID=26419|title=High-Resolution Coronal Imager Photographs the Sun in UV Light at 19.3nm Wavelength|publisher=AZonano.com|date=January 24, 2013|accessdate= February 9, 2013}}</ref>
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| ===The Earth's magnetosphere===
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| [http://clusterlaunch.esa.int/science-e/www/area/index.cfm?fareaid=8 New measurements from the Cluster mission] for the first time now can determine unambiguously the scale sizes of magnetic reconnection in the Earth's [[magnetosphere]], both on the dayside [[magnetopause]] and in the [[magnetotail]]. [[Cluster mission|Cluster]] is a four-spacecraft mission, with the four spacecraft in a tetrahedron arrangement, to separate spatial from temporal changes as the suite flies through space. Cluster has now also unambiguously discovered 'reverse reconnection' near the polar cusps. 'Dayside reconnection' allows interconnection of the Earth's magnetic field with that of the Sun (the [[Interplanetary Magnetic Field]]), allowing particle and energy entry into the Earth's vicinity. Tail reconnection allows release of energy stored in the Earth's magnetic tail, injecting particles deep into the magnetosphere, causing auroral [[substorm]]s. 'Reverse reconnection' is reconnection of Earth's tail magnetic fields with northward Interplanetary Magnetic Fields, causing sunward convection in the Earth's [[ionosphere]]. The upcoming [[Magnetospheric Multiscale Mission]] will improve on Cluster results by having a tighter constellation of spacecraft, allowing finer spatial measurements and finer time detail. In this way the behavior of the electrical currents in the electron diffusion region will be better understood.
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| On 26 February 2008, [[THEMIS]] probes were able to determine, for the first time, the triggering event for the onset of magnetospheric substorms.<ref>[http://www.nasa.gov/mission_pages/themis/auroras/themis_power.html NASA - THEMIS Satellites Discover What Triggers Eruptions of the Northern Lights<!-- Bot generated title -->]</ref> Two of the five probes, positioned approximately one third the distance to the Moon, measured events suggesting a magnetic reconnection event 96 seconds prior to Auroral intensification.<ref>[http://www.sciencemag.org/cgi/content/abstract/1160495 Tail Reconnection Triggering Substorm Onset<!-- Bot generated title -->]</ref> Dr. Vassilis Angelopoulos of the University of California, Los Angeles, who is the principal investigator for the THEMIS mission, claimed, "Our data show clearly and for the first time that magnetic reconnection is the trigger.".<ref>[http://www.space.com/scienceastronomy/080724-themis-aurora-mystery.html Secret of Colorful Auroras Revealed | Space.com<!-- Bot generated title -->]</ref>
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| ===Laboratory Plasma Experiments===
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| The process of magnetic reconnection has been studied in detail by dedicated laboratory experiments, such as the Magnetic Reconnection Experiment (MRX) at Princeton Plasma Physics Laboratory (PPPL). Experiments such as these have confirmed many aspects of magnetic reconnection, including the Sweet-Parker model in regimes where this model is applicable.<ref>{{cite journal|last=Ji|first=H.|coauthors=et al.|title=Magnetic reconnection with Sweet-Parker characteristics in two-dimensional laboratory plasmas|journal=Physics of Plasmas|date=May 1999|volume=6|issue=5|pages=1743|doi=10.1063/1.873432|bibcode = 1999PhPl....6.1743J }}</ref>
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| The confinement of plasma in devices such as [[tokamak]]s, [[spheromak]]s, and [[reversed field pinch]]es requires the presence of closed magnetic flux surfaces. By changing the magnetic topology, magnetic reconnection degrades confinement by disrupting these closed flux surfaces, allowing the hot central plasma to mix with cooler plasma closer to the wall.{{Citation needed|date=January 2012}}
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| ==See also==
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| *[[Current sheet]]
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| *[[Solar corona]]
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| *[[List of plasma (physics) articles]]
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| ==References==
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| * Eric Priest, Terry Forbes, ''Magnetic Reconnection'', Cambridge University Press 2000, ISBN 0-521-48179-1, [http://assets.cambridge.org/0521481791/sample/0521481791WSN01.pdf contents and sample chapter online]
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| * [http://www.space.com/businesstechnology/080206-tw-magnetic-reconnection.html Discoveries about magnetic reconnection in space could unlock fusion power], Space.com, ''6 February 2008''
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| * [http://mms.space.swri.edu Nasa MMS-SMART mission], The Magnetospheric Multiscale (MMS) mission, Solving Magnetospheric Acceleration, Reconnection, and Turbulence. Due for launch in 2014.
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| * [http://clusterlaunch.esa.int/science-e/www/area/index.cfm?fareaid=8 Cluster spacecraft science results]
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| {{reflist}}
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| == External links==
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| * [http://solar-center.stanford.edu/magnetism/magnetismsun.html Magnetism on the Sun]
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| * [http://mrx.pppl.gov/ Magnetic Reconnection Experiment (MRX)]
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| {{DEFAULTSORT:Magnetic Reconnection}}
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| [[Category:Plasma physics]]
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| [[Category:Stellar phenomena]]
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| [[Category:Solar phenomena]]
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