Calculate Fractional Abundance of HI,HII,H- & e- for Hydrogen

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SUMMARY

The calculation of fractional abundance for HI, HII, H-, and e- in hydrogen at a temperature of 5770K and a density of 1017 cm-3 involves analyzing spectral lines. A stronger absorption line indicates a higher concentration of the corresponding species at that wavelength. This method is crucial for understanding the ionization states and electron presence in the photosphere of hydrogen.

PREREQUISITES
  • Understanding of spectral line analysis
  • Knowledge of ionization states of hydrogen
  • Familiarity with thermodynamic principles at 5770K
  • Basic concepts of plasma physics
NEXT STEPS
  • Research methods for spectral line analysis in astrophysics
  • Study the ionization equilibrium of hydrogen species
  • Learn about the impact of temperature and density on ionization
  • Explore computational tools for modeling plasma states
USEFUL FOR

Astrophysicists, researchers in plasma physics, and students studying stellar atmospheres will benefit from this discussion on calculating the fractional abundance of hydrogen species.

goleafsgo113
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how can i calculate the fractional abundance of HI, HII, H- and e- for hydrogen in the photosphere (T=5770K) and density 10^17?
 
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Analysis of spectrum lines, A stronger line in a particular location means there is a lot of that substance to absorb at that particular wavelength.
 

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