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Balmer Series Formula:
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The Balmer series describes the set of spectral line emissions of the hydrogen atom when an electron transitions from a higher energy level (n ≥ 3) to the second energy level (n = 2). These transitions result in visible light emissions.
The calculator uses the Balmer series formula:
Where:
Explanation: The formula calculates the wavelength of light emitted when an electron drops from energy level n to level 2 in a hydrogen atom.
Details: The Balmer series is fundamental in atomic physics and spectroscopy. It helped validate quantum theory and is used in astronomical spectroscopy to identify hydrogen in stars and galaxies.
Tips: Enter the quantum number n (must be an integer ≥ 3). The calculator will output the wavelength in both meters and nanometers.
Q1: What are the visible wavelengths in the Balmer series?
A: The first four lines (n=3-6) produce visible light: Hα (656.3 nm, red), Hβ (486.1 nm, blue-green), Hγ (434.0 nm, blue), and Hδ (410.2 nm, violet).
Q2: Why is n limited to values ≥ 3?
A: The Balmer series specifically refers to transitions to the n=2 level from higher levels. Transitions to n=1 form the Lyman series (UV), and to n=3 form the Paschen series (IR).
Q3: What is the Rydberg constant?
A: The Rydberg constant (1.097×10⁷ m⁻¹) is a physical constant relating to atomic spectra. It represents the limiting value of the highest wavenumber of any photon that can be emitted from hydrogen.
Q4: Can this formula be used for other elements?
A: The basic form works for hydrogen-like atoms (ions with only one electron), but requires modification of the Rydberg constant for different nuclear charges.
Q5: What is the significance of the Balmer series in astronomy?
A: Balmer lines are used to classify stars, measure redshifts, and study stellar atmospheres. The strength of these lines indicates stellar temperature and composition.