7.5
The planetary model describes the hydrogen atom as a tiny solar system, with the electron orbiting a positively-charged nucleus.
Classical physics suggests that because the electron is a charged particle moving in a circular orbit, it should continuously radiate energy while spiraling into the positively-charged nucleus. Eventually, the atom would collapse.
However, this isn’t observed. Atoms are stable.
Niels Bohr proposed that there are orbits at certain, fixed distances from the nucleus. These orbits are numbered integers labeled by the principal quantum number, n. The orbit closest to the nucleus is n = 1. n can be any positive integer, but never zero.
As n increases, so does the radius of the orbital. An electron that is farther away from the nucleus experiences a weaker electrostatic force and is less tightly attracted to the proton.
Each orbit corresponds to a particular energy level or state. The levels are quantized, meaning no energies in between are possible.
An electron at its lowest, most stable energy state, at n = 1, is said to be at its ground state.
The higher energy states, where n > 1, are called the excited states.
An electron can only move to a different energy state either when it absorbs energy — and jumps to a higher level — or when it transitions back down to a lower energy state and releases excess energy in the form of a photon.
The energy absorbed — or emitted — is related to the difference in energy between the final and initial energy levels.
Electrons relaxing from a higher energy level emit shorter-wavelength light than electrons relaxing from a lower energy level.
Although Bohr’s model is suitable only for hydrogen or single electron ions, it set the groundwork for more accurate atomic models.
Following the work of Ernest Rutherford and his colleagues in the early twentieth century, the picture of atoms consisting of tiny dense nuclei surrou…
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