This article has multiple issues. Please help improve it or discuss these issues on the talk page. (Learn how and when to remove these template messages)(Learn how and when to remove this template message)
Neutronium (sometimes shortened to neutrium, also referred to as neutrite) is a hypothetical substance composed purely of neutrons. The word was coined by scientist Andreas von Antropoff in 1926 (before the discovery of the neutron) for the conjectured "element of atomic number zero" that he placed at the head of the periodic table. However, the meaning of the term has changed over time, and from the last half of the 20th century onward it has been also used to refer to extremely dense substances resembling the neutron-degenerate matter theorized to exist in the cores of neutron stars; hereinafter "degenerate neutronium" will refer to this. Science fiction and popular literature frequently use the term "neutronium" to refer to a highly dense phase of matter composed primarily of neutrons.
Neutronium and neutron stars
Neutronium is used in popular literature to refer to the material present in the cores of neutron stars (stars which are too massive to be supported by electron degeneracy pressure and which collapse into a denser phase of matter). This term is very rarely used in scientific literature, for three reasons: there are multiple definitions for the term "neutronium"; there is considerable uncertainty over the composition of the material in the cores of neutron stars (it could be neutron-degenerate matter, strange matter, quark matter, or a variant or combination of the above); the properties of neutron star material should depend on depth due to changing pressure (see below), and no sharp boundary between the crust (consisting primarily of atomic nuclei) and almost protonless inner layer is expected to exist.
When neutron star core material is presumed to consist mostly of free neutrons, it is typically referred to as neutron-degenerate matter in scientific literature.
Neutronium and the periodic table
The term "neutronium" was coined in 1926 by Andreas von Antropoff for a conjectured form of matter made up of neutrons with no protons or electrons, which he placed as the chemical element of atomic number zero at the head of his new version of the periodic table. It was subsequently placed in the middle of several spiral representations of the periodic system for classifying the chemical elements, such as those of Charles Janet (1928), E. I. Emerson (1944), John D. Clark (1950) and in Philip Stewart's Chemical Galaxy (2005).
Although the term is not used in the scientific literature either for a condensed form of matter, or as an element, there have been reports that, besides the free neutron, there may exist two bound forms of neutrons without protons. If neutronium were considered to be an element, then these neutron clusters could be considered to be the isotopes of that element. However, these reports have not been further substantiated.
- Mononeutron: An isolated neutron undergoes beta decay with a mean lifetime of approximately 15 minutes (half-life of approximately 10 minutes), becoming a proton (the nucleus of hydrogen), an electron and an antineutrino.
- Dineutron: The dineutron, containing two neutrons was unambiguously observed in the decay of beryllium-16, in 2012 by researchers at Michigan State University. It is not a bound particle, but had been proposed as an extremely short-lived state produced by nuclear reactions involving tritium. It has been suggested to have a transitory existence in nuclear reactions produced by helions that result in the formation of a proton and a nucleus having the same atomic number as the target nucleus but a mass number two units greater. The dineutron hypothesis had been used in nuclear reactions with exotic nuclei for a long time. Several applications of the dineutron in nuclear reactions can be found in review papers. Its existence has been proven to be relevant for nuclear structure of exotic nuclei. A system made up of only two neutrons is not bound, though the attraction between them is very nearly enough to make them so. This has some consequences on nucleosynthesis and the abundance of the chemical elements.
- Trineutron: A trineutron state consisting of three bound neutrons has not been detected, and is not expected to exist even for a short time.
- Tetraneutron: A tetraneutron is a hypothetical particle consisting of four bound neutrons. Reports of its existence have not been replicated.
- Pentaneutron: Calculations indicate that the hypothetical pentaneutron state, consisting of a cluster of five neutrons, would not be bound.
Although not called "neutronium", the National Nuclear Data Center's Nuclear Wallet Cards lists as its first "isotope" an "element" with the symbol n and atomic number Z = 0 and mass number A = 1. This isotope is described as decaying to element H with a half life of ±0.02 min. 10.24
Free neutrons decay with a half-life of 10 minutes and 11 seconds. While this lifetime is long enough to permit the study of neutronium's chemical properties, there are serious practical problems. Having no charge or electrons, neutronium would not interact with ordinary low-energy photons (light) and would feel no electrostatic forces, so it would diffuse into the walls of any container made of ordinary matter. In the presence of other elements, low energy (thermal) neutrons readily undergo neutron capture to form heavier (and often radioactive) isotope of the element. Neutronium is left off of most periodic tables.
Neutron matter at standard pressure and temperature is predicted by the ideal gas law to be less dense than even hydrogen, with a density of only 45 mg L−1. Similar to helium, neutron matter is predicted to remain gaseous down to absolute zero at normal pressures, as the zero-point energy of the system is too high to allow condensation. At higher temperatures, neutron matter will condense with sufficient pressure, and solidify with even greater pressure. Such pressures exist in neutron stars, where the extreme pressure causes the neutron matter to become degenerate. A teaspoon of degenerate neutronium matter would have a mass of two billion tonnes, and if moved to standard temperature and pressure, would emit 57 yottajoules of β− decay energy in the first half-life (average of 95 ZW of power). This energy may be absorbed as the neutronium gas expands. However, in the presence of atomic matter compressed to the state of electron degeneracy, the β− decay may be inhibited due to the Pauli exclusion principle, thus making free neutrons stable. Also, elevated pressures should make neutrons degenerate themselves. Compared to ordinary elements, neutronium should be more compressible due to the absence of electrically charged protons and electrons. This makes neutronium more energetically favorable than (positive-Z) atomic nuclei and leads to their conversion to (degenerate) neutronium through electron capture, a process which is believed to occur in stellar cores in the final seconds of the lifetime of massive stars, where it is facilitated by cooling via
e emission. As a result, degenerate neutronium can have[clarification needed] a density of ×1017 kg/m3, 4 roughly 13 magnitudes denser than the densest known ordinary substances. It was theorized that extreme pressures of order 100 MeV/Fermi3 may deform the neutrons into a cubic symmetry, allowing tighter packing of neutrons, or cause a strange matter formation.
The term "neutronium" has been popular in science fiction since at least the middle of the 20th century. It typically refers to an extremely dense, incredibly strong form of matter. While presumably inspired by the concept of neutron-degenerate matter in the cores of neutron stars, the material used in fiction bears at most only a superficial resemblance, usually depicted as an extremely strong solid under Earth-like conditions, or possessing exotic properties such as the ability to manipulate time and space. In contrast, all proposed forms of neutron star core material are fluids and are extremely unstable at pressures lower than that found in stellar cores. According to one analysis, a neutron star with a mass below about 0.2 solar masses will explode.
- "Neutrium: The Most Neutral Hypothetical State of Matter Ever". io9.com. 2012. Retrieved 2013-02-11.
- Zhuravleva, Valentina (2005). Ballad of the Stars: Stories of Science Fiction, Ultraimagination, and TRIZ. Technical Innovation Center, Inc. ISBN 9780964074064.
- von Antropoff, A. (1926). "Eine neue Form des periodischen Systems der Elementen" (PDF). Zeitschrift für Angewandte Chemie. 39 (23): 722–725. doi:10.1002/ange.19260392303.
- Stewart, P. J. (2007). "A century on from Dmitrii Mendeleev: Tables and spirals, noble gases and Nobel prizes". Foundations of Chemistry. 9 (3): 235–245. doi:10.1007/s10698-007-9038-x.
- Angelo, J. A. (2006). Encyclopedia of Space and Astronomy. Infobase Publishing. p. 178. ISBN 978-0-8160-5330-8.
- Timofeyuk, N. K. (2003). "Do multineutrons exist?". Journal of Physics G. 29 (2): L9. arXiv: . Bibcode:2003JPhG...29L...9T. doi:10.1088/0954-3899/29/2/102.
- Schirber, M. (2012). "Nuclei Emit Paired-up Neutrons". Physics. 5: 30. Bibcode:2012PhyOJ...5...30S. doi:10.1103/Physics.5.30.
- Spyrou, A.; Kohley, Z.; Baumann, T.; Bazin, D.; et al. (2012). "First Observation of Ground State Dineutron Decay: 16Be". Physical Review Letters. 108 (10): 102501. Bibcode:2012PhRvL.108j2501S. doi:10.1103/PhysRevLett.108.102501. PMID 22463404.
- Bertulani, C. A.; Baur, G. (1986). "Coincidence Cross-sections for the Dissociation of Light Ions in High-energy Collisions" (PDF). Nuclear Physics A. 480 (3–4): 615–628. Bibcode:1988NuPhA.480..615B. doi:10.1016/0375-9474(88)90467-8. Archived from the original (PDF) on 2011-07-20.
- Bertulani, C. A.; Canto, L. F.; Hussein, M. S. (1993). "The Structure And Reactions Of Neutron-Rich Nuclei" (PDF). Physics Reports. 226 (6): 281–376. Bibcode:1993PhR...226..281B. doi:10.1016/0370-1573(93)90128-Z. Archived from the original (PDF) on 2011-09-28.
- Hagino, K.; Sagawa, H.; Nakamura, T.; Shimoura, S. (2009). "Two-particle correlations in continuum dipole transitions in Borromean nuclei". Physical Review C. 80 (3): 1301. arXiv: . Bibcode:2009PhRvC..80c1301H. doi:10.1103/PhysRevC.80.031301.
- MacDonald, J.; Mullan, D. J. (2009). "Big Bang Nucleosynthesis: The Strong Nuclear Force meets the Weak Anthropic Principle". Physical Review D. 80 (4): 3507. arXiv: . Bibcode:2009PhRvD..80d3507M. doi:10.1103/PhysRevD.80.043507.
- Kneller, J. P.; McLaughlin, G. C. (2004). "The Effect of Bound Dineutrons upon BBN". Physical Review D. 70 (4): 3512. arXiv: . Bibcode:2004PhRvD..70d3512K. doi:10.1103/PhysRevD.70.043512.
- Bertulani, C. A.; Zelevinsky, V. (2002). "Is the tetraneutron a bound dineutron-dineutron molecule?". Journal of Physics G. 29 (10): 2431. arXiv: . Bibcode:2003JPhG...29.2431B. doi:10.1088/0954-3899/29/10/309.
- Timofeyuk, N. K. (2002). "On the existence of a bound tetraneutron". arXiv: .
- Bevelacqua, J. J. (1981). "Particle stability of the pentaneutron". Physics Letters B. 102 (2–3): 79–80. Bibcode:1981PhLB..102...79B. doi:10.1016/0370-2693(81)91033-9.
- "Neutrinos give neutron stars a chill". Ars Technica OpenForum. Retrieved 4 December 2013.
- Zarkonnen (2002). "Neutronium". Everything2.com. Retrieved 2013-02-11.
- Felipe J. Llanes-Estrada; Gaspar Moreno Navarro (2011). "Cubic neutrons". Modern Physics Letters A. 27 (6): 1250033. arXiv: . Bibcode:2012MPLA...2750033L. doi:10.1142/S0217732312500332.
- K. Sumiyoshi; S. Yamada; H. Suzuki; W. Hillebrandt (21 Jul 1997). "The fate of a neutron star just below the minimum mass: does it explode?". Max-Planck-Institut für Astrophysik, Germany; RIKEN, U. Tokyo, and KEK, Japan. arXiv: .
Given this assumption... the minimum possible mass of a neutron star is 0.189 (solar masses)