You are partially correct, antoniseb.

I make observation-driven conclusions. When there are no observational data, I try to avoid speculations.

If you will offer explanations for the six observations posted above, I will try to come up with a more complete list of experimental observations - with no conclusions - that gradually led us to the iron-rich Sun - - - an object in which we had no initial interest.

This is not a new finding. The Sun was widely believed to be iron-rich. Development of the H-bomb and adoption of the Hydrogen-filled Sun occurred after the end of Word War II. See:

http://web.umr.edu/~om/AASWashington2002.pdf

To calculate statistical probability, antoniseb, you may want to take a table of abundances in the Sun's photosphere to a statistician. Imagine you go to the Sun, B) stick in a probe, and pull out one atom. What is the probability that atom will be Fe or O or Si or Ni or S or Mg or Ca (any one of the seven elements that make up 99% of the material in ordinary meteorites). These are all trace elements in the photosphere, so the probability of getting any one of them will be quite low. Now you repeat that process six times. Please report your results back here.

Yet the empirical mass-fractionation equation defined by isotope abundances in the solar wind,

log ( f ) = 4.56 log (H/L), where f = fractionation, H = mass of heavy particle, L = mass of light particle,

selects all seven of these trace elements out of the Sun's H-rich photosphere in a single step.

1.) Is this magic, antoniseb? Or

2.) Are elements, as well as isotopes, mass fractionated in the Sun?

Please post your answer.

With kind regards,

Oliver
http://www.umr.edu/~om