Body
NormanI wonder if, in a down to earth , practical manner, the connect/re-connect plays a role in, for instance, the Kromery, where one slides the magnets at right angles to their locked together state.Initially, I need both hands to grasp the flywheel to turn my Kromery.Once turning, one finger's friction on the rim, easily rotates the flywheel, regardless of the load.
Too fast, then eddy currents start warming the magnetic coil cores.Are we cutting those magnetic lines?Cheers Warren
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On Wed, 9 Jan 2019 at 9:25 AM, Norman Wootan [email protected] [EVGRAY]<[email protected]> wrote:
http://young.caltech.edu/Collisionless_Magnetic_Reconnection.html
On 1/9/2019 8:21 AM, Norman Wootan wrote:
https://phys.org/news/2017-10-hidden-mechanics-magnetic-field-reconnection.html
On 1/9/2019 8:14 AM, Norman Wootan wrote:
https://gss.pppl.gov/talks/reconnection%20lecture%201.pdf
On 1/9/2019 8:09 AM, Norman Wootan wrote:
https://link.springer.com/chapter/10.1007%2F978-94-009-0545-0_14
Recent Developments in the Theory of Magnetic Reconnection Dieter Biskamp Max-Planck-Institut fiir Plasmaphysik 8046 Garching bei Miinchen, Federal Republic of Germany Abstract The talk briefly reviews previous stationary models, mainly configurations of the Petschek type, pointing out their shortcomings and basic failure in accounting for fast magnetic reconnection in the limit of large magnetic Reynolds number. It is shown that in this limit no relevant stationary states exist. Instead strong small-scale MHD turbulence develops even in 2D geometry, giving rise to energy dissipation and reconnection rates independent of the value of the collisional re- sistivity. I Introduction In the last decade it has been realized that the presence of magnetic fields is a ubiquitous phenomenon in cosmic systems. On the one hand, magnetic fields serve as a large energy reservoir which may be tapped in a fast dynamic process leading to various kinds of explosive events such as flares. On the other hand, magnetic fields tend to be compressed in processes such as protostar formation and are computed to dominate the dynamics in the later phases in a nonrealistic way if not dissipated sufficiently fast. To account for such processes of fast magnetic field annihilation is the main objective of the theory of magnetic reconnect ion. The term magnetic reconnect ion refers to the picture of magnetic field lines. These have a well-defined meaning in a highly conducting fluid, viz. thin magnetic flux tubes which are carried along with the fluid, maintaining their individuality, though they may be wound in a very complex manner. Only owing to finite electrical resistivity or some equivalent process may two field lines coming close together lose their identities by being cut and reconnected in a different way. Though this is a local process, it leads to a change of field topology permitting new types of large-scale plasma motions that would otherwise be inhibited. The 255 w. BrinbMnn et al. (eds.J, Physical Processes in Hot Cosmic PlIlsmas, 255-269. e 1990 Kluwer Academic Publishers. 256 change of the magnetic field is described by Faraday's law: oB ( ... ) 2'" 7it=VX iixB + 'IV B. (1) Here the ratio of the diffusion term and the convection term (2) is a convenient dimensionless measure of the resistivity, Rm being the magnetic Reynolds number. In practically all astrophysical plasmas Rm is large, essentially because of the large scales L. Hence magnetic diffusion is in general a very weak process. Magnetic processes such as solar flares, however, seem to require fast reconnection with time scales practically independent of Rm. The main theoretical problem therefore is to find models allowing sufficiently high reconnect ion rates. Fast reconnection is not a diffuse process, but is strongly localized in current sheets. Such current sheets may arise at any point with non-vanishing magnetic shear and a velocity gradient along the direction of the shear perpendicular to the field, i.e. virtually everywhere in the plasma, as visualized in Fig. 1. The simplest models are quasi-stationary configurations with one current sheet at a well defined location determined by the overall geometry, which have been investigated in the conventional theory of magnetic reconnection. The basic assumption in these theoretical approaches is the existence of a two-dimensional subsystem around an X-type magnetic neutral point which is small compared with the global magnetic configuration but large compared with the so-called diffusion region around the neutral point, where the diffusion term in (1) is important. In this subsystem conditions would rapidly adjust to changes in the global configuration, so that the evolution of the latter would correspond to a sequence of stationary states in the former which are steady-state solutions with the boundary conditions determined by the global system. This is the idea of stationary forced reconnection. The prototype of such configurations is Petschek's reconnection model 1), which is given schematically in Fig. 2. In fact, much of the theoretical work on magnetic reconnection 2 ),3) consists of modifications and refinements of this model. The theory is based on the effect that the motion of a plasma may be supersonic at arbitrarily low speed with respect to the slow mode . Hence, by analogy with a system of two supersonic gas jets
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