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Old November 4th 03, 03:44 PM
Joseph Lazio
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Default Galaxies without dark matter halos?

"g" == greywolf42 writes:

g Joseph Lazio wrote in message
g ...

Yes, you have "provided [...] two physical mechanisms that can
equalize the motion of neutral hydrogen with EM-driven motion of
ionized hydrogen." You have not shown that these physical
mechanisms operate or are important in the interstellar medium.


g I gave you the standard text by Tayler, and excerpts from same.

I finally had the chance to look at Tayler. I'll confess, I don't
understand why you reference it.


g The reasons are given in the posts where I reference Tayler:
g [invocations of pressure equilibrium]
g In short, I mention Tayler because the book identifies a local
g mechanism -- pressure equalization between gas regions -- that
g causes gas regions to move together. Regardless of which region is
g doing the 'driving.'

As I've pointed out, and as Tayler discusses in Chap. 6, pressure
equilibrium only applies on global scales, length scales much larger
than those relevant for the interfaces between neutral and ionized
regions.

In Chapter 2 he discusses rotation velocities of stars and gas
within the Galaxy. He cites a couple of different estimates of
stellar rotational velocities, which are between 200 and 300 km/s.
He also provides rotation curves derived from gas motions, which
are in the range 220--240 km/s. No major discrepancy here, as
Steve Willner has already pointed out.


g Perhaps you could look a little more closely at those estimates of
g stellar rotation. You'll see they are all based on measuring gas
g or O and B stars (recently condensed from same). As I have
g repeatedly pointed out.

I have looked closely at Tayler's discussion. I see no explicit
mention of stellar types, but the methods he describes seem to rely on
late-type stars (so A, F, G, etc.). One method he describes is
measuring the velocity of the Local Standard of Rest, which is defined
by stars in the solar neighborhood (so mostly late-type stars),
relative to globular clusters (which again are late-type stars).
Later in the chapter he describes measuring the Oort A and B constants
"from nearby stars," which are mostly late-type stars, and obtaining a
rotational velocity of 220 km/s.

* You've asserted that there are plasma filaments with "typical
widths on the order of AU to thousands of AU," but you've
provided no observational evidence for them.


g What type of secondary 'observational' evidence would you accept,
g since we can't directly observe such without an interstellar probe?

Why can't you just provide what you think to be the evidence?


g Because the moderator literally will not allow mention of that
g subject or references for same in this newsgroup. [Long rant on
g sci.astro.research moderator, but no mention of evidence....]

g If interested, see: [...]

I just don't see how many of these are relevant. The only mention of
plasma filaments comes in a discussion of jets from galaxy cores. I
don't see how that relates to the motion of gas in our Galaxy, and in
any event the length scales are parsecs, much larger than what you'd like.

Moreover, Tayler describes magnetic fields in Chapter 6, citing
values similar to what John Park assumed (length scales ~ 100 pc
and field strengths ~ few microGauss). You've objected to both of
these values,

[...]
g Again, it is not the *length* of the filament that is the critical
g dimension, but the thickness that is important.

Where does Tayler discuss filaments at all?




Admittedly, I was browsing through Tayler's text after midnight
last night. I could have missed something. Perhaps you might
provide a succinct summary of your idea (and the evidence
supporting it?) to clear up the confusion?


g Already done. Several times.

g Perhaps you could actually think about the physical dynamics of the
g situation. Instead of attempting to find a word-for-word authority
g for my position.

I'm getting the increasing sense that this is pointless. I think I
have made a good faith effort to read what you've written and read
what you reference.

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