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the paschen series of hydrogen (n=3) can contribute to the visible continuum for the sun since the series limit occurs at 820.8nm. However, it is contribution from the H- ion that dominates the formation of the continuum. using the results of problem 1 above, along with the boltzmann equation, estimate the ratio of the number of H- ions to hydrogen atoms in the n=3 state. using the Saha equation, calculate the ratio of H-ions to neutral hydrogen atoms in the sun's photosphere. Take the temperature of the gas to be the effective temperature, and assume that the electron pressure is 1.5 N/m^3.

the paschen series of hydrogen (n=3) can contribute to the visible continuum for the sun since the series limit occurs at 820.8nm. However, it is contribution from the H- ion that dominates the formation of the continuum. using the results of problem 1 above, along with the boltzmann equation, estimate the ratio of the number of H- ions to hydrogen atoms in the n=3 state. using the Saha equation, calculate the ratio of H-ions to neutral hydrogen atoms in the sun's photosphere. Take the temperature of the gas to be the effective temperature, and assume that the electron pressure is 1.5 N/m^3.

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the paschen series of hydrogen (n=3) can contribute to the visible continuum for the sun since the series limit occurs at 820.8nm. However, it is contribution from the H- ion that dominates the formation of the continuum. using the results of problem 1 above, along with the boltzmann equation, estimate the ratio of the number of H- ions to hydrogen atoms in the n=3 state. using the Saha equation, calculate the ratio of H-ions to neutral hydrogen atoms in the sun's photosphere. Take the temperature of the gas to be the effective temperature, and assume that the electron pressure is 1.5 N/m^3.
Transcribed Image Text:the paschen series of hydrogen (n=3) can contribute to the visible continuum for the sun since the series limit occurs at 820.8nm. However, it is contribution from the H- ion that dominates the formation of the continuum. using the results of problem 1 above, along with the boltzmann equation, estimate the ratio of the number of H- ions to hydrogen atoms in the n=3 state. using the Saha equation, calculate the ratio of H-ions to neutral hydrogen atoms in the sun's photosphere. Take the temperature of the gas to be the effective temperature, and assume that the electron pressure is 1.5 N/m^3.
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