Difference between revisions of "55Fe vs cosmics"
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From Sauli's | From Sauli's | ||
| − | + | [http://books.google.com/books?id=ieMrqqJbaMsC&lpg=PA79&ots=EjIWabWBzx&dq=principles%20of%20operation%20of%20multiwire%20proportional%20and%20drift%20chambers%20sauli&pg=PA79#v=onepage&q=principles%20of%20operation%20of%20multiwire%20proportional%20and%20drift%20chambers%20sauli&f=false|| Principles of operation of multiwire proportional and drift chambers], | |
| − | + | energy loss at atmospheric pressure for minimum ionizing particles is 2.44 keV/cm in Ar and 3.01 keV/cm in CO<sub>2</sub> so for a 50/50 mix, and the shortest path through one straw (1.6 cm), cosmics should deposit a total of 4.4keV at a rate of 2.7 keV/cm. | |
The 55Fe source xrays are the K shell xrays from 55Mn at 6.0 keV. | The 55Fe source xrays are the K shell xrays from 55Mn at 6.0 keV. | ||
Revision as of 13:53, 8 November 2010
From Sauli's Principles of operation of multiwire proportional and drift chambers,
energy loss at atmospheric pressure for minimum ionizing particles is 2.44 keV/cm in Ar and 3.01 keV/cm in CO2 so for a 50/50 mix, and the shortest path through one straw (1.6 cm), cosmics should deposit a total of 4.4keV at a rate of 2.7 keV/cm.
The 55Fe source xrays are the K shell xrays from 55Mn at 6.0 keV.
(The 55Fe decays by electron capture to 55Mn which de-excites by x-ray emission; Kα at 5.9 keV or Kβ X-ray at 6.5 keV with relative intensity 150:42 (Kaye&Laby 1973(!)) so the intensity-weighted average is (5.90*100+5.89*50+6.49*42)/192= 6.0 keV.)
The x-rays undergo photoelectric absorption by 40Ar; Ar emits a photoelectron and then de-excites either by Auger emission (87%) or fluorescence (13%); fluorescence produces the Ar escape peak at 3.0keV when the initial photoelectron causes an avalanche but the 3keV photon does not.
3keV electrons have a range of ~ 100 um in Ar (Sauli) which at a uniform rate of deposition (bad approximation to give a rough idea) is 300 keV/cm and 100 x greater than that for cosmics.
