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The first ionization energy of Carbon is 11.26 eV. Ionized carbon affects the spectral lines observed mostly in cooler stars. It plays a role in the formation of molecular bands like CH, CN, and C2 in stellar atmospheres.

The ionization energy of Hydrogen is 13.6 eV. It is the energy required to remove an electron from a neutral hydrogen atom. This ionization energy contributes to the distinct Balmer series of lines seen in stellar spectra.

The first ionization energy of Nitrogen is 14.53 eV. Ionized nitrogen can affect stellar spectra through emission or absorption lines, and is particularly useful in the study of massive, hot stars where it's used as a diagnostic for temperature and density.

The first ionization energy of Iron is 7.90 eV. Iron lines are very prominent in stellar spectra due to its numerous energy levels and are key for studying stellar population and composition, especially in cooler stars.

The first ionization energy of Silicon is 8.15 eV. Ionized silicon contributes to the Si II lines which can be seen in the spectra of various stars and are notably strong in the spectra of hotter stars.

The ionization energy of Helium is 24.6 eV for the first electron and 54.4 eV for the second. It causes He I and He II lines to appear in star spectra, which are significant for understanding stellar composition.

The first ionization energy of Magnesium is 7.65 eV. The ionized magnesium lines, especially the Mg II doublet near 2800 Å, are prominent in stellar spectra and are used to study the chromospheres of stars.

The first ionization energy of Neon is 21.56 eV. It is inert and does not form lines in spectra under normal conditions, but in high-energy environments, ionized neon contributes to the neon spectral lines which can be used as tracers in certain types of stars.

The first ionization energy of Sodium is 5.14 eV. The easily ionized sodium atoms give rise to the Sodium D lines in star spectra, these are doublet lines at about 5890 Å and 5896 Å, and are strong in the spectra of cool stars.