What is the Mass of Ionized Hydrogen in Stars and How Does it Affect Pressure?

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SUMMARY

The mass of ionized hydrogen in stars is defined as 0.5 AMU, which accounts for the average mass of particles in stellar environments, particularly in the context of pressure calculations within the sun. This value is derived from the mass of a proton, with adjustments for the presence of free electrons and heavier elements like helium. The pressure inside the sun can be calculated using the formula P=((density)/(avg mass of a particle))*kT, where the average mass of a particle is approximately 0.61 AMU when factoring in additional elements. In stellar plasma, the contributions from ion gas and free electron gas are significant, while photon gas pressure is comparatively negligible.

PREREQUISITES
  • Understanding of atomic mass units (AMU)
  • Familiarity with the ideal gas law and pressure calculations
  • Knowledge of stellar composition, including hydrogen and helium
  • Basic principles of plasma physics and quantum mechanics
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Astronomers, astrophysicists, and students studying stellar physics will benefit from this discussion, particularly those interested in the dynamics of pressure in stars and the properties of ionized gases.

Trebor0808
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Could anyone please explain why in the book The Physics of Stars it states that the mass of ionized Hydrogen is 0.5AMU, I cannot figure out why it isn't 1.0078AMU minus the mass of an electron?
 
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Good question, the mass of ionised hydrogen is just that of a proton (with corrections to account for deuterium and tritium). Can you provide the context?
 
It's with regards to the pressure inside the sun, P=((density)/(avg mass of a partice))*kT where the avg mass of a particle in this case is 0.5 AMU. Assuming that the sun is made up entirely of Hydrogen in this case (comes out to be 0.61AMU when taking into account helium and other heavier elements).
 
Trebor0808 said:
It's with regards to the pressure inside the sun, P=((density)/(avg mass of a partice))*kT where the avg mass of a particle in this case is 0.5 AMU. Assuming that the sun is made up entirely of Hydrogen in this case (comes out to be 0.61AMU when taking into account helium and other heavier elements).
In that case you are averaging over the free electrons and the hydrogen nuclei, I would guess. The mass is negligible in comparison to the hydrogen nuclei, so for the same number of electrons and nuclei, the average is half that of the hydrogen nuclei.
 
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Oh okay that does make more sense now, thank you for your help.
 
In calculating the pressure, you need to consider what particles are exerting the pressure. When dilute enough, the plasma inside the star is a mixture of ion gas, free electron gas, and photon gas. But the photon pressure is usually orders smaller. So you only need to consider electron and ion gases.

*In fact, I think in some of the stars the quantum density is such that electrons are already degenerate. This means you have to use Fermi gas pressure for the contribution from electrons.
 
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