Doubly ionized oxygen: Difference between revisions

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These [[emission line]]s were first discovered in the spectra of planetary nebulae in the 1860s. At that time, they were thought to be due to a new element which was named ''[[nebulium]]''. In 1927, [[Ira Sprague Bowen]] published the current explanation identifying their source as doubly ionized oxygen.<ref>{{cite journal | doi = 10.1038/120473a0 | title = The Origin of the Nebulium Spectrum | year = 1927 | author = Bowen, I. S. | journal = Nature | volume = 120 | issue = 3022 | pages = 473|bibcode = 1927Natur.120..473B }}</ref>

Other transitions include the forbidden 88.4&nbsp;μm- and 51.8&nbsp;μm-wavelength transitions in the far [[infrared]] region.<ref name="Osterbrock">{{cite book |last1=Osterbrock |first1=Donald E. |title=Astrophysics of gaseous nebulae and active galactic nuclei |date=1989 |publisher=University Science Books |___location=Mill Valley, Calif. |isbn=0935702229 |page=73}}</ref>

Permitted lines of O III lie in the Middlemiddle [[Ultravioletultraviolet]] band and are hence inaccessible to terrestrial astronomy.

== See also ==