Edmund Clifton StonerFRS (2 October 1899 – 27 December 1968) was a British theoreticalphysicist. He is principally known for his work on the origin and nature of itinerantferromagnetism (the type of ferromagnetic behaviour associated with pure transition metals like cobalt, nickel, and iron), including the collective electron theory offerromagnetism and theStoner criterion forferromagnetism.[3][4][5][6][7][8] Stoner made significant contributions to the electron configurations in theperiodic table.[9][10][11]
Stoner was born in Esher, Surrey, the son of cricketerArthur Hallett Stoner. He won a scholarship toBolton School (1911–1918) and then attendedEmmanuel College, Cambridge, graduating with a degree in natural sciences in 1921.[12] After graduation, he worked at theCavendish Laboratory on the absorption ofX-rays by matter andelectron energy levels; his 1924 paper on this subject prefigured thePauli exclusion principle.[13][10] Stoner was appointed a Lecturer in the Department ofPhysics at theUniversity of Leeds in 1932, becoming Professor of Theoretical Physics in 1939. Starting in 1938, he developed the collective electron theory offerromagnetism. DuringWWII he collaborated with his studentE. P. Wohlfarth and P. Rhodes on the development of high-coercivity magnetic materials fornewly-developed magnetrons and managed the university department while the official head was seconded to government service away from the Leeds.[14] From 1951 to 1963, he held the Cavendish Chair of Physics.[15] He retired in 1963.
A schematic band structure for the Stoner model of ferromagnetism. An exchange interaction has split the energy of states with different spins, and states near the Fermi level are spin-polarized.
Electron bands can spontaneously split into up and down spins. This happens if the relative gain inexchange interaction (the interaction of electrons via the Pauli exclusion principle) is larger than the loss in kinetic energy.
where is the energy of the metal before exchange effects are included, and are the energies of the spin up and down electron bands respectively. The Stoner parameter which is a measure of the strength of the exchange correlation is denoted, the number of electrons is. Finally, is thewavenumber as the electrons bands are in wavenumber-space. If more electrons favour one of the states, this will create ferromagnetism. The electrons obeyFermi–Dirac statistics so when the above formulas are summed over all-space, theStoner criterion for ferromagnetism can be established.
Stoner, Edmund C. (1924). "LXXIII. The distribution of electrons among atomic levels".The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science.48 (286):719–736.doi:10.1080/14786442408634535.ISSN1941-5982.
Stoner, Edmund C. (1929). "V.The limiting density in white dwarf stars".The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science.7 (41):63–70.doi:10.1080/14786440108564713.ISSN1941-5982.[16]
Stoner, Edmund C. (1930). "LXXXVII.The equilibrium of dense stars".The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science.9 (60):944–963.doi:10.1080/14786443008565066.ISSN1941-5982.
^Stoner, E. C. (1939). "Collective Electron Ferromagnetism. II. Energy and Specific Heat".Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences.169 (938):339–371.Bibcode:1939RSPSA.169..339S.doi:10.1098/rspa.1939.0003.
^Stoner, E. C. (1938). "Collective Electron Ferromagnetism".Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences.165 (922):372–414.Bibcode:1938RSPSA.165..372S.doi:10.1098/rspa.1938.0066.
^Kragh, Helge. “Niels Bohr’s Second Atomic Theory.” Historical Studies in the Physical Sciences, vol. 10, University of California Press, 1979, pp. 123–86,https://doi.org/10.2307/27757389.
^abManjit Kumar, Quantum: Einstein, Bohr and the Great Debate About the Nature of Reality, 2008.
^Stoner, Edmund C. (1924). "LXXIII. The distribution of electrons among atomic levels".The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science.48 (286):719–736.doi:10.1080/14786442408634535.ISSN1941-5982.
^The Historical Register of the University of Cambridge Supplement, 1921-30. Cambridge: Cambridge University Press. 1932. p. 158.
^abStoner, Edmund C. (1929). "V.The limiting density in white dwarf stars".The London, Edinburgh, and Dublin Philosophical Magazine and Journal of Science.7 (41):63–70.doi:10.1080/14786440108564713.ISSN1941-5982.