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Sulfur (16 S) has 23 known isotopes with mass numbers ranging from 27 to 49, four of which are stable: 32 S (95.02%), 33 S (0.75%), 34 S (4.21%), and 36 S (0.02%). The preponderance of sulfur-32 is explained by its production from carbon-12 plus successive fusion capture of five helium-4 nuclei, in the so-called alpha process of exploding type II supernovas (see silicon burning).
This is an accepted version of this page This is the latest accepted revision, reviewed on 21 February 2025. This article is about the chemical element. For other uses, see Sulfur (disambiguation). Chemical element with atomic number 16 (S) Sulfur, 16 S Sulfur Alternative name Sulphur (pre-1992 British spelling) Allotropes see Allotropes of sulfur Appearance Lemon yellow sintered microcrystals ...
There are no stable nuclides with mass numbers 5 or 8. There are stable nuclides with all other mass numbers up to 208 with the exceptions of 147 and 151, which are represented by the very long-lived samarium-147 and europium-151. (Bismuth-209 was found to be radioactive in 2003, but with a half-life of 2.01 × 10 19 years.)
The mass of the nuclide (in daltons) is A (m n − E / k) where E is the energy, m n is 1.008664916 Da and k = 931.49410242 the conversion factor between MeV and daltons. half-life column The main column shows times in seconds (31,556,926 seconds = 1 tropical year ); a second column showing half-life in more usual units (year, day) is also ...
An even number of protons or neutrons is more stable (higher binding energy) because of pairing effects, so even–even nuclides are much more stable than odd–odd. One effect is that there are few stable odd–odd nuclides: in fact only five are stable, with another four having half-lives longer than a billion years.
In the atomic symbol of 32 S, the number 32 refers to the mass of each sulfur atom in daltons, the result of the 16 protons and 16 neutrons of 1 dalton each that make up the sulfur nucleus. The three rare stable isotopes of sulfur are 34 S (4.2% of natural sulfur), 33 S (0.75%), and 36 S (0.015%). [ 4 ]
U.S. Coast Guard Cutter Waesche crewmembers offload bales of seized narcotics in San Diego, Feb. 13, 2025. / Credit: U.S. Coast Guard photo by Petty Officer 3rd Christopher Sappey
After a star completes the oxygen burning process, its core is composed primarily of silicon and sulfur. [23] If it has sufficiently high mass, it further contracts until its core reaches temperatures in the range of 2.7–3.5 billion K (230–300 keV). At these temperatures, silicon and other isotopes suffer photoejection of nucleons by ...