How do the pressure broadening and Stark broadening of spectral lines provide information about the density and electric fields in astronomical environments?
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what is n in chemistry
- Can two electrons in the same atom have the same value of n?
- In astrophysics, how are the spectra of stars used to determine their composition and temperature, and how does the understanding of atomic energy levels (based on n) play a role?
- How do the spectral lines emitted by plasmas relate to transitions between energy levels with different n values in the ions present?
- How does the concept of isoelectronic species (atoms or ions with the same number of electrons) relate to their electron configurations and the filling of energy levels with specific n values?
- How can the ionization energy of an atom be determined from its Rydberg series limit?
- How does the filling of these orbitals according to Hund's rule and the Pauli Exclusion Principle lead to the electron configurations of elements?
- How does the absorption of light by biomolecules (e.g., chlorophyll, hemoglobin) involve transitions between electronic energy levels with different n values?
- In the Paschen series, what is the final value of n?
- How does the g-factor in EPR relate to the spin and orbital angular momentum of the unpaired electron, which are influenced by its quantum numbers including n and l?
- How can an electron move from one energy level (with a certain n) to another?
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