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  • 1
    Electronic Resource
    Electronic Resource
    Electric-drift generated trajectories and particle acceleration in collisionless magnetic reconnection (1997)
    [S.l.] : American Institute of Physics (AIP)
    Physics of Plasmas 4 (1997), S. 2261-2268 
    Details
    ISSN: 1089-7674
    Source: AIP Digital Archive
    Topics: Physics
    Notes: Adiabatic acceleration of charged particles along magnetic field lines originates from the coupling between the electric drift and longitudinal motion in a nonunidirectional magnetic field. As a result, initially slow particles entering the reconnection site of an X-type magnetic geometry can leave the latter as substantially accelerated jets directed along the magnetic separatrices. The corresponding energy spectrum has a power-law form, with the spectral index depending on the angle between the separatrices. © 1997 American Institute of Physics.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1063/1.872555
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  • 2
    Electronic Resource
    Electronic Resource
    Nonlinear magnetic reconnection with collisionless dissipation (1995)
    [S.l.] : American Institute of Physics (AIP)
    Physics of Plasmas 2 (1995), S. 3169-3178 
    Details
    ISSN: 1089-7674
    Source: AIP Digital Archive
    Topics: Physics
    Notes: An analytical model of two-dimensional collisionless reconnection in an X-type magnetic geometry is presented. The conversion of magnetic energy to the kinetic energy of accelerated ions takes place in the vicinity of the neutral line. The structure of this dissipation region and the magnetic energy release rate have been investigated both for linear and nonlinear regimes of collisionless reconnection. A simple model of global reconnection flow has been constructed, assuming an incompressible ideal magnetohydrodynamics approximation outside the dissipation region. The corresponding scaling for the external Mach number (Me) is found, which predicts a maximum reconnection rate Me=1/2R˜m −1/2, where R˜m≈(Le/λi)2(very-much-greater-than)1 is the effective magnetic Reynolds number for collisionless reconnection (Le is the global size of the system and λi is the ion inertial skin depth). © 1995 American Institute of Physics.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1063/1.871149
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  • 3
    Electronic Resource
    Electronic Resource
    Energy release and plasma heating by forced magnetic reconnection (1998)
    [S.l.] : American Institute of Physics (AIP)
    Physics of Plasmas 5 (1998), S. 1506-1513 
    Details
    ISSN: 1089-7674
    Source: AIP Digital Archive
    Topics: Physics
    Notes: A simple model of forced magnetic reconnection in a force-free magnetic field is considered, which allows the calculation of the magnetic energy release during the current sheet reconnection. The dependence of this energy on characteristics of the magnetic configuration has been studied, and it was found that the released energy becomes very large when the field is near the marginal tearing stability. A persistent plasma heating provided by ongoing external driving and internal reconnection is most efficient when the time-scales of these processes are comparable. Possible implications of the obtained results for the problem of solar coronal heating are briefly discussed. © 1998 American Institute of Physics.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1063/1.872809
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  • 4
    Electronic Resource
    Electronic Resource
    Magnetic reconnection and energy release in the solar corona by Taylor relaxation (1991)
    Springer
    Solar physics 131 (1991), S. 297-318 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The heating of the solar corona by resistive turbulence of coronal magnetic fields is considered. The theory of this process, based on the Taylor-Heyvaerts-Priest hypothesis and a magnetic relaxation equation, is developed. Such an approach allows one to obtain the successive magnetic reconnection configurations and energy balance of the coronal magnetic field in response to prescribed motions of the photospheric footpoints. Two specific models of the coronal magnetic configuration are investigated, namely an array of closely packed flux tubes and a two-dimensional magnetic arcade.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151640
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  • 5
    Electronic Resource
    Electronic Resource
    Reconnective release of magnetic energy in astrophysical plasmas (1994)
    Springer
    Space science reviews 68 (1994), S. 15-28 
    Details
    ISSN: 1572-9672
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Two particular examples are considered of astrophysical objects containing a highly conducting tenuous plasma with an excess magnetic energy supplied by an external source. The first example is the solar corona, whose magnetic field is continuously distorted by footpoint shuffling due to photospheric motions. The second case it an extragalactic jet extending from a galactic nucleus with an immersed magnetic field, and which is perturbed by variations in the pressure of the external medium. In both cases it is assumed that the system tends towards its lowest magnetic energy equilibrium via magnetic reconnection, thus providing a fast release of injected magnetic energy. Explicit relations between the characteristics of the external driver and the magnetic energy dissipation rate in these objects have been obtained. The relevance of this mechanism for heating the solar corona and maintaining radio emission from extragalactic jets is then. discussed by comparing these results with observational data.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00749113
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  • 6
    Electronic Resource
    Electronic Resource
    Coronal magnetic field evolution under reconnective relaxation (1994)
    Springer
    Space science reviews 70 (1994), S. 303-307 
    Details
    ISSN: 1572-9672
    Keywords: Sun ; Corona ; Magnetic reconnection
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The nonlinear evolution of a partially open coronal magnetic configuration is considered, assuming that corona responds to photospheric footpoint motions by small-scale reconnection events that produce a relaxed lower-energy state while conserving the global magnetic helicity of the system. The results of numerical calculations for such a relaxed equilibrium show an essential role of the amount of helicity injected to the closed-field region. If photospheric perturbations are incoherent (small-scale shearing with inefficient helicity injection), the relaxed state becomes close to an initial potential field. In this case reconnective relaxation does not result in a substantial global evolution, just providing heating of the corona (Vekstein et al, 1993). On the contrary, sufficient injection of the magnetic helicity can lead to a considerable restructuring of the coronal magnetic configuration, with possible change of its topology (formation of magnetic islands), and even catastrophic loss of equilibrium (Wolfson et al, 1994)
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00777885
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