Body
Good question Warren! Nobody really knows how the potential and
current manifest in the conductor passing through a flux field. Your
question is valid cause there very well may be some sort of reconnect
occurring here. Theory was, that the flux field was photon stream which
enabled pairing to produce electrons and attending current. There is
still so much that we don't know but things are getting interesting.
Read that last doc that I posted for it is very enlightening on this
subject. See: http://www.tfcbooks.com/mall/more/temp/x565-hen.htm
This is one of Oles favorites.
On 1/9/2019 9:09 AM, Warren Keillor [email protected]
[EVGRAY] wrote:
>
> Norman
>
> I 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
> Sent from Yahoo Mail on Android
> <https://go.onelink.me/107872968?pid=InProduct&c=Global_Internal_YGrowth_AndroidEmailSig__AndroidUsers&af_wl=ym&af_sub1=Internal&af_sub2=Global_YGrowth&af_sub3=EmailSignature>
>
> 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
>
>