- Giovanni and Dennis,

> The scattering from molecules and very tiny particles (< 1 /10

While most people thend to do so, there's actually no reason to distinguish

> wavelength) is predominantly Rayleigh scattering. For particle sizes

> larger than a wavelength, Mie scattering predominates. This pretty

> much covers particles *smaller* than 5 microns, doesn't it?

large particles (a ~ lambda) from smaller ones (a < lambda) since Mie scattering

describes them as well.

But now to the point. Goivanni wrote:

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the point is that even accounting for the contribution of all particle sizes 5

microns and below, there is *too much* light contribution visible on that tail

features. Then the question: where is all the mass that makes such details

visible? This is the question to answer...

------------------------------------------

I don't know why you want to have more mass.

Assume we have a dust particle of a certain size Ro (volume Vo) and mass mo.

This particle fragments into n smaller particles of size r (volume V), where n =

Vo/V = Ro^3/r^3. What happens if we observe this?

Along the line of view, the particle column density N is defined as

N = mc/m

where mc is the column mass density mc=s*rho=s*m/V (rho ist the (solid state)

density of the dust, s is the column length). Thus, we obtain

N = mc/m = (s*m/V)/m = s/V

Let Adust be the geometrical cross section of the dust particles (Adust~r^2).

For the intensity of scattering, the scattering cross section (or scattering

efficiency) A_sca is the important parameter:

A_sca ~ N*Adust ~ Adust/V ~ 1/r

The conclusion of this is: If you take one dust grain and fragment it, the

scattering cross section increases, i.e., the scattering intensifies (I~A_sca).

(Btw, the basic princliple of the above mentioned is hidden in Sekanina & Farell

(1980)).

So, as long as you destroy large particles of the order of 10micron into

particles of the order of 0.1-1 micron (Mie regime for visual wavelengths), the

above holds. If the particles are smaller and you run into the Rayleigh regime,

you probably lose a lot of intensity in the visual and won't see scattered light

from this dust anymore. This means that you only see the larger particles in the

striae. Assuming typical collision or break-up power law distributions of grain

sizes (i.e., number of particles of size r is proportional to size r^-x), I

would draw the following conclusions:

* Stiae should be brighter than their "parent synchrones/syndynes" (this is

laxly formulated but I hope you understand what I mean)

* a power law distribution for the grain sizes as a result of breakup implies a

"fade-in" from the position of break-up (Mie regime) and a "fade-out" when the

particles become to small (Rayleigh regime).

Cheers,

Sebastian

--

-------------------------------

Sebastian F. Hoenig

Max-Planck-Institut fuer Radioastronomie

Auf dem Huegel 69

53121 Bonn

Phone +49 (0) 228 525 188

Fax +49 (0) 228 525 437

Skype: sfhoenig

------------------------------- - Dear Sebastian,

OK in all points, but you cannot forget, as you do,

the syndynes. That of 10 micron is MILLION km

far (inside towards the head of the comet) with

respect to the locus where all striae clearly start,

which is a syndyne of ONE-TWO microns!!

We must take into account all the factors, also those that (unfotunatley) contradict our beloved theory.

I remind you something similar happened with

Comet West: Sekanina analysed the striae photometry,

and was forced to conclude, in order to match the tail

and striae brightness, that the original parents where

needles meter long with a section of one micron

aligned to sun direction, in order to have beta close to

one (cross section of one micron) and enough mass to

produce the striae. Here for sure the situation is even

worse, and who can believe to such needles ??

Cheers,

Giovanni

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