AST 111 Lecture Notes - Lecture 18: Niels Bohr, Uncertainty Principle, Werner Heisenberg

• School: Tunxis Community College
• Department: Astronomy
• Course: AST 111
• Professor: Bourne

Document Summary

A hot dense glowing object ( a hot solid, liquid, or high density gas) will emit a continuous, black body-like spectrum: a low density gas will emit light of certain wavelengths, a bright line, or emission line spectrum. When light having a continuous spectrum passes through a cooler gas, dark lines appear superimposed upon the continuous spectrum. For a given element, the dark absorption and bright emission lines were found at the exact same wavelengths. Johannes balmer- in 1885devised an empirical formula for which the wavelength spacing in the different lines of the hydrogen spectrum could be observed. Planck"s 1900 quantum formula suggested that a single emission line corresponded to photons of only one wavelength, frequency, or energy. Lord rutherford- proposed the atom model in 1911 that had positive charge in the middle, and negative charge surrounding the positive charge.