Body
Moray, Jon Gentry and Warren asked pertinent questions regarding
velocities, magnetic flux etc. in plasma events so I did a search as to
whether Alfven waves have a frequency. This site pretty well defines a
lot of plasma info that we need. See:
https://www.britannica.com/science/plasma-state-of-matter#ref507092
On 1/10/2019 6:29 AM, Warren Keillor [email protected]
[EVGRAY] wrote:
> Norman
> Hooper's work looks very compelling. At his time of experimentation,
> super conductors were not a reality as they are now. The fact that a
> resistance free conductor might accelerate a potential's velocity,
> after going through a resistor, suggests an analogy to fluid dynamics,
> much like Bernuili's principle application of a venturi to gases.
> The idea of dielectric conductors is a mind smasher, inverting our
> entire circuit thoughts.
> Generally, pretty radical concepts, in a zone to set us up for quantum
> physics thinking. Whew!
> 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 3:17 PM, Norman Wootan [email protected] [EVGRAY]
> <[email protected]> wrote:
>
> 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]
> <mailto:[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]
>> <mailto:[email protected]> [EVGRAY]
>> <[email protected]> <mailto:[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
>>
>