Discussion Overview
The discussion revolves around the mass of ionized hydrogen in stars and its implications for pressure calculations, particularly in the context of stellar physics. Participants explore the relationship between particle mass, density, and pressure within stars, specifically focusing on the Sun.
Discussion Character
- Technical explanation
- Conceptual clarification
- Debate/contested
Main Points Raised
- One participant questions why the mass of ionized hydrogen is stated as 0.5 AMU instead of the expected 1.0078 AMU minus the mass of an electron.
- Another participant suggests that the mass of ionized hydrogen is effectively that of a proton, with considerations for isotopes like deuterium and tritium.
- It is noted that the average mass of a particle in the Sun's context is 0.5 AMU, assuming a hydrogen-dominated composition, which changes to 0.61 AMU when accounting for helium and heavier elements.
- A participant elaborates that the average mass is derived from averaging the masses of free electrons and hydrogen nuclei, indicating that the mass of electrons is negligible compared to hydrogen nuclei.
- Another participant emphasizes the need to consider the types of particles exerting pressure in the star, mentioning the roles of ion gas, free electron gas, and photon gas, with the latter being less significant.
- There is a suggestion that in some stars, the quantum density may lead to degenerate electrons, requiring the use of Fermi gas pressure for electron contributions.
Areas of Agreement / Disagreement
Participants express varying interpretations of the mass of ionized hydrogen and its implications for pressure calculations, indicating that multiple views remain without a clear consensus on the specifics.
Contextual Notes
Some assumptions regarding the composition of stars and the treatment of particle masses in pressure calculations are not fully resolved, particularly concerning the contributions of different particle types and the conditions under which they operate.