Observational studies of reconnection in the solar corona

McKenzie, David E.
November 2011
Physics of Plasmas;Nov2011, Vol. 18 Issue 11, p111205
Academic Journal
In recent years, observational studies of the corona have shifted focus. Where they were once purely qualitative morphological explorations seeking to support the presence of reconnection, more investigations are providing empirical estimates of the physical conditions in the reconnecting corona. These studies are enabled and enhanced by orbiting telescopes with high angular and temporal resolution. In this article, some recent findings about the empirical quantities are reviewed, including recent estimates of the flux transferred in individual patchy reconnection episodes, the size distribution of post-reconnection flux tubes, and the energy released by the flux tubes as they shrink.


Related Articles

  • Observational Evidence for Rising Penumbral Flux Tubes? Jurčák, J.; Sobotka, M. // Solar Physics;Apr2007, Vol. 241 Issue 2, p223 

    On 13 May 2000 parts of a penumbra were observed in an active region NOAA 8990 with the La Palma Stokes Polarimeter attached to the Swedish Vacuum Solar Telescope. The stratification over the solar atmosphere of different physical parameters is retrieved from these data by using the Stokes...

  • Flux and Field Line Conservation in 3-D Non-Ideal MHD Flows: Remarks About Criteria for 3-D Reconnection Without Magnetic Neutral Points and Their Application to the Heliospheric Interface. Nickeler, D. H.; Fahr, H.-J. // Solar Physics;May2006, Vol. 235 Issue 1/2, p191 

    In this paper, we address the issue of finding velocity fields which conserve magnetic flux or at least magnetic fieldline connectivity. We start from the basic principles of flux and line conservation and present and discuss the criterion, given by Newcomb (1958), Stern (1966), and Vasyliunas...

  • Macro-particle simulations of collisionless magnetic reconnection. Tanaka, Motohiko // Physics of Plasmas;Aug95, Vol. 2 Issue 8, p2920 

    Studies the basic process of collisionless reconnection in terms of coalescence of two flux bundles. Use of an implicit particle simulation of two-dimensions; Significant toroidal acceleration and streaming of the electrons without direct thermalization in the current sheet; Insensitivity of...

  • Magnetohydrodynamic processes in the solar corona: Flares, coronal mass ejections, and magnetic... Low, B.C. // Physics of Plasmas;May94, Vol. 1 Issue 5, p1684 

    Reports on the evolution of the magnetized, million-degree solar corona in cycles of about 11 years, in dynamical response to generated magnetic fluxes emerging from below to eventually reverse global magnetic polarity. Focus on the creation, stability and eventual eruption of structures from...

  • New Views of Sun's Corona.  // Science Teacher;Mar2013, Vol. 80 Issue 3, p18 

    The article discusses a rocket mission launched in July 2012 which used a High-resolution Coronal Imager (Hi-C) to examine the the solar atmosphere, or corona, of the Sun and found that a process known as magnetic reconnection causes the extreme temperatures of the corona.

  • Chromospheric anemone jets and magnetic reconnection in partially ionized solar atmosphere. Singh, K. A. P.; Shibata, K.; Nishizuka, N.; Isobe, H. // Physics of Plasmas;Nov2011, Vol. 18 Issue 11, p111210 

    The solar optical telescope onboard Hinode with temporal resolution of less than 5 s and spatial resolution of 150 km has observed the lower solar atmosphere with an unprecedented detail. This has led to many important findings, one of them is the discovery of chromospheric anemone jets in the...

  • Reciprocatory magnetic reconnection in a coronal bright point. Zhang, Q. M.; Chen, P. F.; Ding, M. D.; Ji, H. S. // Astronomy & Astrophysics / Astronomie et Astrophysique;Aug2014, Vol. 568, p1 

    Context. Coronal bright points (CBPs) are small-scale and long-duration brightenings in the lower solar corona. They are often explained in terms of magnetic reconnection. Aims. We aim to study the substructures of a CBP and clarify the relationship among the brightenings of different patches...

  • Plasma Flows in Coronal Streamers—Numerical Simulation. Dumitrache, Cristiana // AIP Conference Proceedings;9/10/2007, Vol. 934 Issue 1, p129 

    Coronal streamers are very interesting, long lived, features of solar corona. They are linked to prominences, CMEs and also to slow solar wind. The have different shape and behavior. We present a numerical simulation of a coronal streamer computed on five solar radii. Vertical motions in the...

  • Numerical Simulations of Dome-Shaped EUV Waves from Different Active-Region Configurations. Selwa, M.; Poedts, S.; DeVore, C. // Solar Physics;Jun2013, Vol. 284 Issue 2, p515 

    Recently, 3D STEREO observations explained the 3D structure of EUV waves. Patsourakos and Vourlidas ( Astrophys. J. 700, L182, ), Veronig et al. ( Astrophys. J. 716, L57, ) and Selwa, Poedts, and DeVore ( Astrophys. J. 747, L21, ) reported on the dome-shaped EUV waves resulting from different...


Read the Article


Sorry, but this item is not currently available from your library.

Try another library?
Sign out of this library

Other Topics