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Hello, as many of you may know I have been trying to develop a simple thermal equilibrium photosphere model to estimate ball park figures for photosphere properties e.g. temperature, thickness, pressure and elemental abundances etc from my own measurements.
It’s always been the pressure component of line profile broadening that has been the hardest to understand, temperature and rotational broadening were easy to get to grips with by comparison.
I have uploaded my latest understanding as documented in the attached Theory.pdf (section 3) and would like comments as to its “correctness”. The definition of the impact parameter has changed from previous versions of this document. Following this revision I will have to modify the papers describing my analyses of various stars however only the actual values of the impact parameters will change all the other properties calculated remain unchanged.
I am planning to attend the 4th June BAA spectroscopy meeting at the IOP if anybody would like to discuss this topic.
Regards
Ken Whight
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