With an accuracy of about .32 parts per billion, the fine-structure constant is approximately 7.2973525664(17)x10-3. It is often stated as its reciprocal, which is 137.035999139(31). These figures are estimates from experimental observation and calculation, but the fine-structure constant has not been reduced to a mathematical equation, and thus it retains an element of theoretical mystery to physicists. This is compounded by the contention of some physicists, using powerful current telescopes, that this constant was slightly different billions of years ago.
= = = = = = = = = = = = = = = = = = = = = = = = = = = = = =
Arnold Sommerfeld introduced the fine-structure constant in 1916, as part of his theory of the relativistic deviations of atomic spectral lines from the predictions of the Bohr model. The first physical interpretation of the fine-structure constant α was as the ratio of the velocity of the electron in the first circular orbit of the relativistic Bohr atom to the speed of light in the vacuum. Equivalently, it was the quotient between the minimum angular momentum allowed by relativity for a closed orbit, and the minimum angular momentum allowed for it by quantum mechanics. It appears naturally in Sommerfeld's analysis, and determines the size of the splitting or fine-structure of the hydrogenic spectral lines.
Is the Fine-Structure Constant Actually Constant?
Physicists have pondered whether the fine-structure constant is in fact constant, or whether its value differs by location and over time. A varying α has been proposed as a way of solving problems in cosmology and astrophysics. String theory and other proposals for going beyond the Standard Model of particle physics have led to theoretical interest in whether the accepted physical constants (not just α) actually vary.
Feynman on the Fine-Structure Constant
Richard Feynman, one of the originators and early developers of the theory of quantum electrodynamics (QED), referred to the fine-structure constant in these terms: