The composition of the atmosphere of Jupiter

Modern studies of the composition of Jupiter’s atmosphere date back to the mid-nineteenth century, when the nearinfrared spectrum of the planet was viewed by Rutherfurd (1863) using diffraction gratings of his own manufacture. He discovered features that remained unidentified until 1932, when Wildt showed that the unknown spectral lines were due to ammonia and methane. In later years, building on the original insight of Jeffreys (1923, 1924), Wildt and others went on to note that the low density of Jupiter and the presence of these hydrogen-rich compounds in the atmosphere were consistent with a bulk composition similar to that of the Sun, that is, primarily hydrogen.