Re: magnetic lines like these

[LUDWIK KOWALSKI <KOWALSKIL@alpha.montclair.edu>]

      Referring to:

> > The main issue is to explain the experimental fact; measurable=
=20
> > magnetic fields were recorded by satellites as far as 100 AU=20
> > from the Sun. How can this happen?=20

      Tim Folkerts <Tim.Folkerts@valpo.edu> writes:

> I had a thought that doesn't especially agree with the text you quo=
ted,=20
> but what about this?
>
> 1)  The sun produces a local magnetic field.
> 2)  This field magnetizes (aligns the magnetic moments of)=20
>     the particles that make up the solar wind. =20
> 3)  As the particles head out, they tend to keep their alignment.
> 4)  These aligned particles contribute to the local magnetic field
>     at distant locations.
> =20
> Think of it as throwing magnets away from the sun!  If you have a b=
unch=20
> of little magnets all pointing the same way, you have a magnetic fi=
eld.=20
> I don't know how well it agrees with actual experiments, but it see=
ms=20
> plausible.

A  plausible model. Why didn't astrophysicist explain data in the sam=
e way
for students? Why do they draw narrow magnetic field loops (not at al=
l like
circles of a dipole) emerging from the Sun and return to it from far =
away=20
places (100 AU)? Magnetic fields of spinning electrons and protons ar=
e=20
confined to regions near these traveling magnets.=20

Clouds of such tiny magnets? Clouds forming chains? Like coils in
a solenoid? =20

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*

         On 5/11/1998, referring to this description of the solar win=
d,
=20
> > ...................................................................
> > "As a plasma moves through a magnetic field, the charged particles =
are
> > trapped in spiral paths along the magnetic field lines. [OK so far.=
]
> > The plasma becomes bound to the magnetic field. At the same time th=
e
> > plasma captures the magnetic field and holds it within the plasma. =
Once
> > an organized flow of charged particles has been set up, it generate=
s its
> > own magnetic field (as does an electromagnet). This field from the =
moving
> > particles maintains the magnetic field that first caused the curren=
t flow.
> > So the original field is reinforced. Then if a plasma moves in bulk=
, it
> > carries the magnetic field lines with it." (Zeilik, 1997, page 160)
> > ...................................................................=
.....

        Chuck Britton <britton@odie.ncssm.edu> wrote:

> The picture I'm visualizing here is a bundle of magnetic flux lines =
that
> have closed into a nearly circular loop. The electric charges are sp=
iraling
> around this loop, sort of around the surface of a doughnut. The magn=
etic
> loop wraps around the hole of the doughnut and the current is always
> flowing through the hole in the same direction and wrapping back alo=
ng the
> outer edge of the doughnut. I suppose that the charge is always eith=
er +=20
> or always - in a given doughnut or the counter moving opposite charg=
es=20
> would interfere with each other???

I can visualize a nearly curcular =D2bundle of magnetic flux lines=
=D3. A single-
wire rectangular loop with a large current has two short segments (on=
e above=20
another, horizontally, for example)> The short segments are separated=
 by very=20
long vertical segments. The current in vertical segments flows in opp=
osite=20
directions and their combined magnetic field is nearly zero everywher=
e. Short=20
segments, on the other hand, are so far away that their fields do not=
 cancel.=20
The field near each short segment is a nearly curcular =D2bundle of m=
agnetic=20
flux lines=D3.And I can imagine electons spiraling around a circular =
bundle of=20
such lines. A toroidal current of electrons, in a vacuum, if you wish=
..=20

But what does this have to do with solar wind? Where are the particle=
s which=20
take the magnetic field from a region near a source (doughnut) to a r=
egion=20
very far away from the source?  High speed electrons passing near the=
=20
doughnut will travers the field, bending a little, and will eventuall=
y travel=20
along straight lines at constant velocities. The magnetic field assoc=
iated=20
with their motion has nothing to do with the magnetic field near the=
=20
daughnut. And in the case of the macroscopically neutral solar wind (=
+ and -=20
particles ejected from the Sun with the same mean speed) the net fiel=
d of=20
escaping particle must be zero. What does Zeilik mean by saying =D2th=
is field=20
=66rom the moving particles maintains the magnetic field that first c=
aused the=20
current  flow=D3? Something is not right with this explanation, I thi=
nk, (or=20
with my physics).
                                  Ludwik Kowalski