Imaging coronal magnetic-field reconnection in a solar flare

  title={Imaging coronal magnetic-field reconnection in a solar flare},
  author={Yang Su and Astrid M. Veronig and Gordon D. Holman and Brian R. Dennis and Tongjiang Wang and Manuela Temmer and Weiqun Gan},
  journal={Nature Physics},
Magnetic-field reconnection is believed to play a fundamental role in magnetized plasma systems throughout the Universe(1), including planetary magnetospheres, magnetars and accretion disks around black holes. This letter presents extreme ultraviolet and X-ray observations of a solar flare showing magnetic reconnection with a level of clarity not previously achieved. The multi-wavelength extreme ultraviolet observations from SDO/AIA show inflowing cool loops and newly formed, outflowing hot… 

Extreme ultraviolet imaging of three-dimensional magnetic reconnection in a solar eruption

The sequence of extreme ultraviolet images clearly shows that two groups of oppositely directed and non-coplanar magnetic loops gradually approach each other, forming a separator or quasi-separator and then reconnecting.

Multi-scale Observation and Data-driven Modeling of Magnetic Reconnection in Flaring Chromospheric Plasmas on the Sun

Magnetic reconnection is a multi-faceted process of energy conversion in astrophysical, space and laboratory plasmas that operates at microscopic scales but has macroscopic drivers and

Three-dimensional magnetic reconnection in a collapsing coronal loop system

Context. Magnetic reconnection is believed to be the primary mechanism by which non-potential energy stored in coronal magnetic fields is rapidly released during solar eruptive events. Unfortunately,


Magnetic reconnection is believed to be the dominant energy release mechanism in solar flares. The standard flare model predicts both downward and upward outflow plasmas with speeds close to the

Observations of Reconnection Flows in a Flare on the Solar Disk

Magnetic reconnection is a well-accepted part of the theory of solar eruptive events, though the evidence is still circumstantial. Intrinsic to the reconnection picture of a solar eruptive event,

Observational evidence of magnetic reconnection in a coronal bright point

Magnetic reconneciton is considered to be the fundamental process by which magnetic energy is converted into plasma or particle kinetic energy. And magnetic reconnection is widly applied as the

Magnetic reconnection research with petawatt-class lasers

Magnetic reconnection is regarded as a fundamental phenomenon in space and laboratory plasmas. It converts magnetic energy to kinetic energy of plasma particles through the topological rearrangements

Fast plasmoid-mediated reconnection in a solar flare

Magnetic reconnection is a multi-faceted process of energy conversion in astrophysical, space and laboratory plasmas that operates at microscopic scales but has macroscopic drivers and consequences.

Observations of Turbulent Magnetic Reconnection within a Solar Current Sheet

Magnetic reconnection is a fundamental physical process in various astrophysical, space, and laboratory environments. Many pieces of evidence for magnetic reconnection have been uncovered. However,

Observing the release of twist by magnetic reconnection in a solar filament eruption

Evidence of fast reconnection in a solar filament eruption is presented using high-resolution H-alpha images from the New Vacuum Solar Telescope, supplemented by extreme ultraviolet observations, to demonstrate a new role for reconnections in solar eruptions: the release of magnetic twist.




Magnetic reconnection changes the magnetic field topology and powers explosive events in astrophysical, space, and laboratory plasmas. For flares and coronal mass ejections (CMEs) in the solar

A loop-top hard X-ray source in a compact solar flare as evidence for magnetic reconnection

SOLAR flares are thought to be the result of magnetic reconnection — the merging of antiparallel magnetic fields and the consequent release of magnetic energy. Flares are classified into two types1:

Direct Observation of High-Speed Plasma Outflows Produced by Magnetic Reconnection in Solar Impulsive Events

Spectroscopic observations of a solar limb flare recorded by SUMER on SOHO reveal for the first time hot, fast magnetic reconnection outflows in the corona. As the reconnection site rises across the

Clear Evidence of Reconnection Inflow of a Solar Flare

We found an important piece of evidence for magnetic reconnection inflow in a flare on 1999 March 18. The flare occurred on the northeast limb, displaying a nice cusp-shaped soft X-ray loop and a

In situ detection of collisionless reconnection in the Earth's magnetotail

The serendipitous encounter of the Wind spacecraft with an active reconnection diffusion region is reported, in which are detected key processes predicted by models of collisionless reconnection in the magnetotail.

Direct Observations of the Magnetic Reconnection Site of an Eruption on 2003 November 18

We report direct observations of the magnetic reconnection site during an eruptive process that occurred on 2003 November 18. The event started with a rapid expansion of a few magnetic arcades

Magnetic Reconnection in the Near Venusian Magnetotail

Observations with the Venus Express magnetometer and low-energy particle detector revealed magnetic field and plasma behavior in the near-Venus wake that is symptomatic of magnetic reconnection, a process that occurs in Earth’s magnetotails but is not expected in the magnetotail of a nonmagnetized planet such as Venus.

Motion of Flare Footpoint Emission and Inferred Electric Field in Reconnecting Current Sheets

A systematic motion of Hα kernels during solar flares can be regarded as the chromospheric signature of progressive magnetic reconnection in the corona, in that the magnetic field lines swept through

Coronal Mass Ejections: Models and Their Observational Basis

Coronal mass ejections (CMEs) are the largest-scale eruptive phenomenon in the solar system, expanding from active region-sized nonpotential magnetic structure to a much larger size. The bulk of

Solar Flares: Magnetohydrodynamic Processes

This paper outlines the current understanding of solar flares, mainly focused on magnetohydrodynamic (MHD) processes responsible for producing a flare. Observations show that flares are one of the