Problem: Part A. What wavelength λ should the astrophysicist look for to detect a transition of an electron from the n = 6 to the n = 3 level? Express your answer with the appropriate units.An astrophysicist working at an observatory is interested in finding clouds of hydrogen in the galaxy. Usually, hydrogen is detected by looking for the Balmer series of spectral lines in the visible spectrum. Unfortunately, the instrument that detects hydrogen emission spectra at this particular observatory is not working very well and only detects spectra in the infrared region of electromagnetic radiation. Therefore, the astrophysicist decides to check for hydrogen by looking at the Paschen series, which produces spectral lines in the infrared part of the spectrum. The Paschen series describes the wavelengths of light emitted by the decay of electrons from higher orbits to the n = 3 level.

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Part A. What wavelength λ should the astrophysicist look for to detect a transition of an electron from the n = 6 to the n = 3 level? 

Express your answer with the appropriate units.


An astrophysicist working at an observatory is interested in finding clouds of hydrogen in the galaxy. Usually, hydrogen is detected by looking for the Balmer series of spectral lines in the visible spectrum. Unfortunately, the instrument that detects hydrogen emission spectra at this particular observatory is not working very well and only detects spectra in the infrared region of electromagnetic radiation. Therefore, the astrophysicist decides to check for hydrogen by looking at the Paschen series, which produces spectral lines in the infrared part of the spectrum. The Paschen series describes the wavelengths of light emitted by the decay of electrons from higher orbits to the n = 3 level.

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Our tutors have indicated that to solve this problem you will need to apply the Bohr and Balmer Equations concept. If you need more Bohr and Balmer Equations practice, you can also practice Bohr and Balmer Equations practice problems.