Talk:Isotopes of fluorine/Archive 1

Archive 1

Nubase 2003

This article is part of Wikipedia:Wikiproject Isotopes. Please keep style and phrasings consistent across the set of pages. For later reference and improved reliability, data from all considered multiple sources is collected here. References are denoted by these letters:

• (A) G. Audi, O. Bersillon, J. Blachot, A.H. Wapstra. The Nubase2003 evaluation of nuclear and decay properties, Nuc. Phys. A 729, pp. 3-128 (2003). — Where this source indicates a speculative value, the # mark is also applied to values with weak assignment arguments from other sources, if grouped together. An asterisk after the A means that a comment of some importance may be available in the original.
• (B) National Nuclear Data Center, Brookhaven National Laboratory, information extracted from the NuDat 2.1 database. (Retrieved Sept. 2005, from the code of the popup boxes).
• (C) David R. Lide (ed.), Norman E. Holden in CRC Handbook of Chemistry and Physics, 85th Edition, online version. CRC Press. Boca Raton, Florida (2005). Section 11, Table of the Isotopes. — The CRC uses rounded numbers with implied uncertainties, where this concurs with the range of another source it is treated as exactly equal in this comparison.
• (D) More specific level data from reference B's Levels and Gammas database.
• (E) Same as B but excitation energy replaced with that from D.

  Z   N refs symbol   half-life                   spin              excitation energy
  9   5 A   |F-14    |                           |2-#
  9   5 B   |F-14    |                           |(2-)
  9   6 A   |F-15    |410(60)E-24 s              |(1/2+)
  9   6 B   |F-15    |[1.0(2) MeV]               |(1/2+)
  9   6 C   |F-15    |[0.9(3) MeV]               |(1/2+)
  9   7 A   |F-16    |11(6)E-21 s                |0-
  9   7 B   |F-16    |[40(20) keV]               |0-
  9   7 C   |F-16    |[0.037(14) MeV]            |0-
  9   8 ABC |F-17    |64.49(16) s                |5/2+
  9   9 AC  |F-18    |109.771(20) min            |1+
  9   9 B   |F-18    |1.8291(4) h                |1+
  9   9 A   |F-18m   |234 ns                     |5+               |1121.36(15) keV
  9   9 D   |F-18m   |162(7) ns                  |5+               |1121.36(15) keV
  9  10 ABC |F-19    |STABLE                     |1/2+
  9  11 A   |F-20    |11.163(8) s                |2+
  9  11 B   |F-20    |11.07(6) s                 |2+
  9  11 C   |F-20    |11.00 s                    |2+
  9  12 ABC |F-21    |4.158(20) s                |5/2+
  9  13 A   |F-22    |4.23(4) s                  |4+,(3+)
  9  13 B   |F-22    |4.23(4) s                  |(4+)
  9  13 C   |F-22    |4.23 s                     |4+
  9  14 AB  |F-23    |2.23(14) s                 |(3/2,5/2)+
  9  14 C   |F-23    |2.2 s                      |5/2+
  9  15 AB  |F-24    |400(50) ms                 |(1,2,3)+
  9  15 C   |F-24    |0.3 s                      |
  9  16 AB  |F-25    |50(6) ms                   |(5/2+)#
  9  16 C   |F-25    |~50 ms                     |
  9  17 AC  |F-26    |10.2(14) ms                |1+
  9  17 B   |F-26    |9.6(8) ms                  |1+
  9  18 A   |F-27    |4.9(2) ms                  |5/2+#
  9  18 B   |F-27    |5.0(2) ms                  |(5/2+)
  9  18 C   |F-27    |5.0 ms                     |
  9  19 AB  |F-28    |<40 ns                     |
  9  20 A   |F-29    |2.6(3) ms                  |5/2+#
  9  20 B   |F-29    |2.5(4) ms                  |(5/2+)
  9  20 C   |F-29    |2.5 ms                     |
  9  21 AB  |F-30    |<260 ns                    |
  9  22 A   |F-31    |1# ms [>260 ns]            |5/2+#
  9  22 B   |F-31    |>260 ns                    |

Femto 15:16, 19 November 2005 (UTC)

Talk

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Should include information about industrial usage, if any. Someone with experience of nuclear physics should verify the contents of the table. jni 07:34, 23 August 2005 (UTC)

I've overwritten the existing table in the course of creating a full set of 'isotopes of' semi-stub articles with masses and abundances. The decay data may be re-included later as part of WikiProject Isotopes. Femto 11:17, 24 August 2005 (UTC)

^18mF

What's that ^18mF entry? I'm reasonably across atomic and nuclear physics, being a professional molecular physicist, and I don't know that I've seen this notation before. That I (who knows a decent amount about this stuff) don't know what it means suggests to me that the average punter will have no idea. Thus an explanatory note and/or link in the table would be appropriate and beneficial. 150.203.35.113 (talk) 04:09, 27 October 2009 (UTC)

Incremental neutron mass values

The incremental mass value given between OE9F17 to OO9F18 is 0.998842 amu's which is more than the incremental mass value given for the change from OO9F18 to OE9F19 (0.997466) This is an unusual high incremental mass value increase for the transition to the OO9F18 atom and an unusual low incremental mass increase value for the OEF19 transition, which is a mass increase of only 0.997466 amu's for the addition of a neutron to the nucleus.WFPM (talk) 01:05, 8 July 2012 (UTC)

Nuclear transition at 0 degrees Kelvin

Where does the OO9F18 atom get the energy at 0 degrees Kelvin to break up a PN nucleon pair (2.23Mev) and then capture an orbital elec tron by the unpaired neutron and then to change to EE8O18?WFPM (talk) 01:24, 6 April 2012 (UTC)

F-18 does not contain an H-2 nucleus (binding energy 2.23MeV), so it dosen't need enough decay energy to break one up. Radioactive decay or any exothermic reaction produces energy by converting to something of lower mass. 18.0009373(5)u - 17.9991596129(8)u = 0.0017777(5)u * 931.494MeV/u = 1.6559(5)MeV. Temperature play no part here as starting with colder F-18 would simply produce colder O-18. This is on the average of many decays as the neutrino produced in EC or e+ emission has variable energy. Darian2 (talk) 04:00, 31 August 2012 (UTC)

Question about fluorine-18

Does anyone know where the trace amount of fluorine-18 found in nature comes from? (On the page for fluorine it's listed as "trace".) Is the fluorine-18 in use from reactors? It would be nice to mention something about this in the article. modify 21:43, 30 October 2015 (UTC)

From cosmic ray spallation of Ar, as well as the reaction ¹⁸O(p,n)¹⁸F. This is given at cosmogenic nuclide. Double sharp (talk) 06:51, 15 April 2017 (UTC)