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In the areas between absorption shells, the distribution usually follows simple power laws, but the shell structure is in general not something which can be neglected.
Format:
CLUSTER FUNCTION cluster_function [N nmax]
Example:
cluster function 1/n**3 n 15
Doing this will produce a warning since, to compute probability to have a cluster size of 0, one would divide by zero.
Additional information on:
Please note that the first number is the probability to have a cluster size of 0, i.e. a cluster without ionisation electrons. When a charged particle traverses a gas, most interactions result only in excitation, not in ionisation. If you set a mean number of clusters per cm which only takes clusters into account that contain at least 1 electron, then you have to set the first probability to 0.
Format:
CLUSTER prob_size0 prob_size1 ... (blank line)
Example:
CLUSTER 0 0 0.1 0.2 0.5 0.2 0.1 0
(Note the blank line)
Format:
CLUSTER FUNCTION cluster_function [N nmax] OVERLAP-TABLE-AND-FUNCTION prob_size0 prob_size1 ... (blank line)
Example:
CLUSTER FUNCTION 21.6/N**2 N=200 OVERLAP 0 86 20 10
There has to be a blank line after the cluster sizes. One can also simulate this format by using a Do loop:
cluster 0 86 20 10 For i From 4 To 200 Do {21.6/i**2} Enddo// (note that the previous line is blank !)
But this would be less efficient since the formula inside the loop (21.6/i**2) is translated each iteration of the loop. Note that there has to be a blank line after Enddo.
A more efficient version of the latter would be:
cluster 0 86 20 10 {21.6/row(200)**2}// (note that the previous line is blank !)
Formatted on 0108-09- at 08:33.