Physics:Isotopes of helium

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Short description: Nuclides with atomic number of 2 but with different mass numbers
Main isotopes of Chemistry:helium (2He)
Iso­tope Decay
abun­dance half-life (t1/2) mode pro­duct
3He 0.0002% stable
4He 99.9998% stable
Standard atomic weight Ar, standard(He)
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Although there are nine known isotopes of helium (2He) (standard atomic weight: 4.002602(2)), only helium-3 (3He) and helium-4 (4He) are stable.[2] All radioisotopes are short-lived, the longest-lived being 6He with a half-life of 806.92(24) milliseconds. The least stable is 10He, with a half-life of 260(40) yoctoseconds (2.6(4)×10−22 s), although it is possible that 2He may have an even shorter half-life.

In the Earth's atmosphere, the ratio of 3He to 4He is 1.343(13)×10−6.[3] However, the isotopic abundance of helium varies greatly depending on its origin. In the Local Interstellar Cloud, the proportion of 3He to 4He is 1.62(29)×10−4,[4] which is 121(22) times higher than that of atmospheric helium. Rocks from the Earth's crust have isotope ratios varying by as much as a factor of ten; this is used in geology to investigate the origin of rocks and the composition of the Earth's mantle.[5] The different formation processes of the two stable isotopes of helium produce the differing isotope abundances.

Equal mixtures of liquid 3He and 4He below 0.8 K separate into two immiscible phases due to differences in quantum statistics: 4He atoms are bosons while 3He atoms are fermions.[6] Dilution refrigerators take advantage of the immiscibility of these two isotopes to achieve temperatures of a few millikelvins.

List of isotopes

Nuclide
 Z N Isotopic mass (u)
[n 1] 		Half-life

[resonance width] 		Decay
mode
[n 2] 		Daughter
isotope
[n 3] 		Spin and
parity
[n 4][n 5] 		Physics:Natural abundance (mole fraction)
Normal proportion Range of variation
2He[n 6] 2 0 2.015894(2) ≪ 10−9 s[7] p (> 99.99%) 1H 0+#
β+ (< 0.01%) 2H
3He[n 7][n 8] 2 1 3.016029321967(60) Stable 1/2+ 0.000002(2)[8] [4.6×10−10, 0.000041][9]
4He[n 7] 2 2 4.002603254130(158) Stable 0+ 0.999998(2)[8] [0.999959, 1.000000][9]
5He 2 3 5.012057(21) 602(22) ys
[758(28) keV] 		n 4He 3/2−
6He[n 9] 2 4 6.018885889(57) 806.92(24) ms β− (99.999722(18)%) 6Li 0+
β−d[n 10] (0.000278(18)%) 4He
7He 2 5 7.027991(8) 2.51(7) zs
[182(5) keV] 		n 6He (3/2)−
8He[n 11] 2 6 8.033934388(95) 119.5(1.5) ms β− (83.1(1.0)%) 8Li 0+
β−n (16(1)%) 7Li
β−t[n 12] (0.9(1)%) 5He
9He 2 7 9.043946(50) 2.5(2.3) zs n 8He 1/2(+)
10He 2 8 10.05281531(10) 260(40) ys
[1.76(27) MeV] 		2n 8He 0+
  1. ↑ ( ) – Uncertainty (1σ) is given in concise form in parentheses after the corresponding last digits.
  2. ↑ Modes of decay:
    n: Neutron emission
    p: Proton emission
  3. ↑ Bold symbol as daughter – Daughter product is stable.
  4. ↑ ( ) spin value – Indicates spin with weak assignment arguments.
  5. ↑ # – Values marked # are not purely derived from experimental data, but at least partly from trends of neighboring nuclides (TNN).
  6. ↑ Intermediate in the proton–proton chainreaction
  7. ↑ 7.0 7.1 Produced during Big Bang nucleosynthesis
  8. ↑ This and 1H are the only stable nuclides with more protons than neutrons
  9. ↑ Has 2 halo neutrons
  10. ↑ d: Deuteron emission
  11. ↑ Has 4 halo neutrons
  12. ↑ t: Triton emission

Helium-2 (diproton)

Helium-2, or 2He, is an extremely unstable isotope of helium. Its nucleus, a diproton, consists of two protons with no neutrons. According to theoretical calculations, it would have been much more stable (although still undergoing β+ decay to deuterium) if the strong interaction had been 2% greater.[10] Its instability is due to spin–spin interactions in the nuclear force and to the quantum mechanics described by the Pauli exclusion principle, which states that within a given quantum system two or more identical particles with the same half-integer spins (that is, fermions) cannot simultaneously occupy the same quantum state—all which presents for helium-2 that its two protons (of the diproton) have opposite-aligned spins and the diproton itself has a negative binding energy.[11]

There may have been observations of 2He. In 2000, physicists first observed a new type of radioactive decay in which a nucleus emits two protons at once—perhaps a 2He nucleus.[12][13] The team led by Alfredo Galindo-Uribarri of the Oak Ridge National Laboratory announced that the discovery will help scientists understand the strong nuclear force and provide fresh insights into the creation of elements inside stars. Galindo-Uribarri and co-workers chose an isotope of neon with an energy structure that prevents it from emitting protons one at a time. This means that the two protons are ejected simultaneously. The team fired a beam of fluorine ions at a proton-rich target to produce 18Ne, which then decayed into oxygen and two protons. Any protons ejected from the target itself were identified by their characteristic energies. There are two ways in which the two-proton emission may proceed. The neon nucleus might eject a "diproton"—a pair of protons bundled together as a 2He nucleus—which then decays into separate protons. Alternatively, the protons may be emitted separately but simultaneously—so-called "democratic decay". The experiment was not sensitive enough to establish which of these two processes was taking place.

More evidence of 2He was found in 2008 at the Istituto Nazionale di Fisica Nucleare, in Italy.[7][14] A beam of 20Ne ions was directed at a target of beryllium foil. This collision converted some of the heavier neon nuclei in the beam into 18Ne nuclei. These nuclei then collided with a foil of lead. The second collision had the effect of exciting the 18Ne nucleus into a highly unstable condition. As in the earlier experiment at Oak Ridge, the 18Ne nucleus decayed into an 16O nucleus, plus two protons detected exiting from the same direction. The new experiment showed that the two protons were initially ejected together, correlated in a quasibound 1S configuration, before decaying into separate protons much less than a nanosecond later.

Further evidence comes from RIKEN in Japan[citation needed] and the Joint Institute for Nuclear Research in Dubna, Russia,[citation needed] where beams of 6He nuclei were directed at a cryogenic hydrogen target to produce 5H. It was discovered that the 6He nucleus can donate all four of its neutrons to the hydrogen.[citation needed] The two remaining protons could be simultaneously ejected from the target as a 2He nucleus, which quickly decayed into two protons. A similar reaction has also been observed from 8He nuclei colliding with hydrogen.[15]

Under the influence of electromagnetic interactions, the Jaffe-Low primitives [16] may leave the unitary cut, creating narrow two-nucleon resonances, like a diproton resonance with a mass of 2000 MeV and a width of a few hundred keV. [17] To search for this resonance, a beam of protons with kinetic energy T = 250 MeV and an energy spread below 100 keV is required, which is feasible considering electron cooling of the beam.

2He is an intermediate in the first step of the proton–proton chainreaction. The first step of the proton–proton chain reaction is a two-stage process; first, two protons fuse to form a diproton:

11H + 11H + 1.25 MeV[citation needed] → 22He,

followed by the immediate beta-plus decay of the diproton to deuterium:

22He → 21D + Positron + Electron Neutrino + 1.67 MeV[citation needed],

with the overall formula

11H + 11H → 21D + e+ + νe + 0.42 MeV[citation needed].

The hypothetical effect of the binding of the diproton on Big Bang and stellar nucleosynthesis has been investigated.[10] Some models suggest that variations in the strong force allowing the existence of a bound diproton would enable the conversion of all primordial hydrogen to helium in the Big Bang, with catastrophic consequences on the development of stars and life. This proposition is used as an example of the anthropic principle. However, a 2009 study suggests that such a conclusion cannot be drawn, as the formed diprotons would still decay to deuterium, whose binding energy would also increase. In some scenarios, it is postulated that hydrogen (in the form of deuterium) could still survive in relatively large quantities, rebutting arguments that the strong force is tuned within a precise anthropic limit.[18]

Helium-3

Main page: Physics:Helium-3

3He is stable and is the only stable isotope other than 1H with more protons than neutrons. (There are many such unstable isotopes, the lightest being 7Be and 8B.) There is only a trace amount (0.000002(2))[8] of 3He on Earth, primarily present since the formation of the Earth, although some falls to Earth trapped in cosmic dust.[5] Trace amounts are also produced by the beta decay of tritium.[19] In stars, however, 3He is more abundant, a product of nuclear fusion. Extraplanetary material, such as lunar and asteroid regolith, has trace amounts of 3He from solar wind bombardment.

For helium-3 to form a superfluid, it must be cooled to a temperature of 0.0025 K, or almost a thousand times lower than helium-4 (2.17 K). This difference is explained by quantum statistics, since helium-3 atoms are fermions, while helium-4 atoms are bosons, which condense to a superfluid more easily.

Helium-4

Main page: Physics:Helium-4

The most common isotope, 4He, is produced on Earth by alpha decay of heavier radioactive elements; the alpha particles that emerge are fully ionized 4He nuclei. 4He is an unusually stable nucleus because its nucleons are arranged into complete shells. It was also formed in enormous quantities during Big Bang nucleosynthesis.

Terrestrial helium consists almost exclusively (0.999998(2))[8] of this isotope. Helium-4's boiling point of 4.2 K is the second lowest of all known substances, second only to helium-3. When cooled further to 2.17 K, it transforms to a unique superfluid state of zero viscosity. It solidifies only at pressures above 25 atmospheres, where its melting point is 0.95 K.

Heavier helium isotopes

Although all heavier helium isotopes decay with a half-life of less than one second, researchers have used particle accelerator collisions to create unusual atomic nuclei for elements such as helium, lithium and nitrogen. The unusual nuclear structures of such isotopes may offer insights into the isolated properties of neutrons and physics beyond the Standard Model.[20][21]

The shortest-lived isotope is helium-10 with a half-life of 260(40) yoctoseconds. Helium-6 decays by emitting a beta particle and has a half-life of 806.92(24) milliseconds. The most widely studied heavy helium isotope is helium-8. This isotope, as well as helium-6, is thought to consist of a normal helium-4 nucleus surrounded by a neutron "halo" (containing two neutrons in 6He and four neutrons in 8He). Halo nuclei have become an area of intense research. Isotopes up to helium-10, with two protons and eight neutrons, have been confirmed. 10He, despite being a doubly magic isotope, has a very short half-life; it is not particle-bound and near-instantaneously drips out two neutrons.[22]

References

  1. ↑ Meija, Juris; Coplen, Tyler B.; Berglund, Michael; Brand, Willi A.; De Bièvre, Paul; Gröning, Manfred; Holden, Norman E.; Irrgeher, Johanna et al. (2016). "Atomic weights of the elements 2013 (IUPAC Technical Report)". Pure and Applied Chemistry 88 (3): 265–91. doi:10.1515/pac-2015-0305. 
  2. ↑ "helium-3 | chemical isotope | Britannica" (in en). https://www.britannica.com/science/helium-3. 
  3. ↑ Sano, Yuji; Wakita, Hiroshi; Sheng, Xu (1988). "Atmospheric helium isotope ratio". Geochemical Journal 22 (4): 177–181. doi:10.2343/geochemj.22.177. Bibcode: 1988GeocJ..22..177S. https://www.jstage.jst.go.jp/article/geochemj1966/22/4/22_4_177/_article. 
  4. ↑ Busemann, H.; Bühler, F.; Grimberg, A.; Heber, V. S.; Agafonov, Y. N.; Baur, H.; Bochsler, P.; Eismont, N. A. et al. (2006-03-01). "Interstellar Helium Trapped with the COLLISA Experiment on the MiR Space Station—Improved Isotope Analysis by In Vacuo Etching" (in en). The Astrophysical Journal 639 (1): 246. doi:10.1086/499223. ISSN 0004-637X. Bibcode: 2006ApJ...639..246B. 
  5. ↑ 5.0 5.1 "Helium Fundamentals". http://www.mantleplumes.org/HeliumFundamentals.html. 
  6. ↑ The Encyclopedia of the Chemical Elements. p. 264. 
  7. ↑ 7.0 7.1 Schewe, Phil (2008-05-29). "New Form of Artificial Radioactivity". Physics News Update (865 #2). http://www.aip.org/pnu/2008/split/865-2.html. 
  8. ↑ 8.0 8.1 8.2 8.3 "Atomic Weight of Helium". Commission on Isotopic Abundances and Atomic Weights. https://ciaaw.org/helium.htm. 
  9. ↑ 9.0 9.1 Meija, Juris; Coplen, Tyler B.; Berglund, Michael; Brand, Willi A.; Bièvre, Paul De; Gröning, Manfred; Holden, Norman E.; Irrgeher, Johanna et al. (2016-03-01). "Isotopic compositions of the elements 2013 (IUPAC Technical Report)" (in en). Pure and Applied Chemistry 88 (3): 293–306. doi:10.1515/pac-2015-0503. ISSN 1365-3075. 
  10. ↑ 10.0 10.1 Bradford, R. A. W. (27 August 2009). "The effect of hypothetical diproton stability on the universe". Journal of Astrophysics and Astronomy 30 (2): 119–131. doi:10.1007/s12036-009-0005-x. Bibcode: 2009JApA...30..119B. http://rickbradford.co.uk/Diprotons.pdf. 
  11. ↑ Nuclear Physics in a Nutshell, C. A. Bertulani, Princeton University Press, Princeton, N.J., 2007, Chapter 1, ISBN:978-0-691-12505-3.
  12. ↑ Physicists discover new kind of radioactivity , in physicsworld.com Oct 24, 2000.
  13. ↑ J. Gómez del Campo et al. (2001). "Decay of a Resonance in 18Ne by the Simultaneous Emission of Two Protons". Physical Review Letters 86 (2001): 43–46. doi:10.1103/PhysRevLett.86.43. PMID 11136089. Bibcode: 2001PhRvL..86...43G. 
  14. ↑ Raciti, G.; Cardella, G.; De Napoli, M.; Rapisarda, E.; Amorini, F.; Sfienti, C. (2008). "Experimental Evidence of 2He Decay from 18Ne Excited States". Phys. Rev. Lett. 100 (19): 192503–192506. doi:10.1103/PhysRevLett.100.192503. PMID 18518446. Bibcode: 2008PhRvL.100s2503R. 
  15. ↑ Korsheninnikov A. A. (2003-02-28). "Experimental Evidence for the Existence of 7H and for a Specific Structure of 8He". Physical Review Letters 90 (8): 082501. doi:10.1103/PhysRevLett.90.082501. PMID 12633420. Bibcode: 2003PhRvL..90h2501K. http://fy.chalmers.se/~f2bmz/papers/korsheninnikov_2003_7h.pdf. 
  16. ↑ Jaffe, R. L.; Low, F. E. (1979). "Connection between quark-model eigenstates and low-energy scattering". Physical Review D 19: 2105-2118. doi:10.1103/PhysRevD.19.2105. https://journals.aps.org/prd/abstract/10.1103/PhysRevD.19.2105. 
  17. ↑ Krivoruchenko, M. I. (2011). "Possibility of narrow resonances in nucleon-nucleon channels". Physical Review C 84: 015206. doi:10.1103/PhysRevC.84.015206. https://journals.aps.org/prc/abstract/10.1103/PhysRevC.84.015206. 
  18. ↑ MacDonald, J.; Mullan, D.J. (2009). "Big Bang Nucleosynthesis: The strong nuclear force meets the weak anthropic principle". Physical Review D 80 (4): 043507. doi:10.1103/PhysRevD.80.043507. Bibcode: 2009PhRvD..80d3507M. 
  19. ↑ K. L. Barbalace. "Periodic Table of Elements: Li—Lithium". EnvironmentalChemistry.com. http://environmentalchemistry.com/yogi/periodic/Li-pg2.html. 
  20. ↑ "Helium-8 study gives insight into nuclear theory, neutron stars | Argonne National Laboratory" (in en). 2008-01-25. https://www.anl.gov/article/helium8-study-gives-insight-into-nuclear-theory-neutron-stars. 
  21. ↑ "Radioactive beams drive physics forward" (in en-GB). 1999-11-29. https://cerncourier.com/a/radioactive-beams-drive-physics-forward/. 
  22. ↑ Clifford A. Hampel (1968). The Encyclopedia of the Chemical Elements. Reinhold Book Corporation. p. 260. ISBN 978-0278916432. https://archive.org/details/encyclopediaofch00hamp. 

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