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In particle physics, the lightest supersymmetric particle (LSP) is the generic name given to the lightest of the additional hypothetical particles found in supersymmetric models. In models with R-parity conservation, the LSP is stable; in other words, it cannot decay into any Standard Model particle, since all SM particles have the opposite R-parity. There is extensive observational evidence for an additional component of the matter density in the universe, which goes under the name dark matter. The LSP of supersymmetric models is a dark matter candidate and is a weakly interacting massive particle (WIMP).

Constraints on LSP from cosmology

The LSP is unlikely to be a charged wino, charged higgsino, slepton, sneutrino, gluino, squark, or gravitino but is most likely a mixture of neutral higgsinos, the bino and the neutral winos, i.e. a neutralino. In particular, if the LSP were charged (and is abundant in our galaxy) such particles would have been captured by the Earth's magnetic field and form heavy hydrogen-like atoms. Searches for anomalous hydrogen in natural water however have been without any evidence for such particles and thus put severe constraints on the existence of a charged LSP.

As a dark matter candidate

Dark matter particles must be electrically neutral; otherwise they would scatter light and thus not be "dark". They must also almost certainly be non-colored. With these constraints, the LSP could be the lightest neutralino, the gravitino, or the lightest sneutrino.

• Sneutrino dark matter is ruled out in the Minimal Supersymmetric Standard Model (MSSM) because of the current limits on the interaction cross section of dark matter particles with ordinary matter as measured by direct detection experiments—the sneutrino interacts via Z boson exchange and would have been detected by now if it makes up the dark matter. Extended models with right-handed or sterile sneutrinos reopen the possibility of sneutrino dark matter by lowering the interaction cross section.
• Neutralino dark matter is the favored possibility. In most models the lightest neutralino is mostly bino (superpartner of the hypercharge gauge boson field B), with some admixture of neutral wino (superpartner of the weak isospin gauge boson field W) and/or neutral Higgsino.
• Gravitino dark matter is a possibility in supersymmetric models in which the scale of supersymmetry breaking is low, around 100 TeV. In such models the gravitino is very light, of order an eV. As dark matter, the gravitino is sometimes called a super-WIMP because its interaction strength is much weaker than that of other supersymmetric dark matter candidates. For the same reason, its direct thermal production in the early universe is too inefficient to account for the observed dark matter abundance. Rather, gravitinos would have to be produced through the decay of the next-to-lightest supersymmetric particle (NLSP).

In extra-dimensional theories, there are analogous particles called LKPs or Lightest Kaluza–Klein Particle. These are the stable particles of extra-dimensional theories.

See also

• Dark matter
• Darkon (unparticle)
• List of hypothetical particles
• Supersymmetry
• Weakly interacting slender particle

References

1. Jungman, Gerard; Kamionkowski, Marc; Griest, Kim (1996). "Supersymmetric dark matter". Phys. Rep. 267 (5–6): 195–373. arXiv:hep-ph/9506380. Bibcode:1996PhR...267..195J. doi:10.1016/0370-1573(95)00058-5. S2CID 119067698.
2. Ellis, John R.; Hagelin, J.S.; Nanopoulos, Dimitri V.; Olive, Keith A.; Srednicki, M. (July 1983). "Supersymmetric Relics from the Big Bang". Nucl. Phys. B238 (2): 453–476. Bibcode:1984NuPhB.238..453E. doi:10.1016/0550-3213(84)90461-9. OSTI 1432463.
3. Byrne, Mark; Kolda, Christopher; Regan, Peter (2002). "Bounds on Charged, Stable Superpartners from Cosmic Ray Production". Physical Review D. 66 (7): 075007. arXiv:hep-ph/0202252. Bibcode:2002PhRvD..66g5007B. CiteSeerX 10.1.1.348.1389. doi:10.1103/PhysRevD.66.075007. S2CID 17073892.
4. Smith, P.F.; Bennett, J.R.J.; Homer, G.J.; Lewin, J.D.; Walford, H.E.; Smith, W.A. (November 1981). "A search for anomalous hydrogen in enriched D2O, using a time-of-flight spectrometer". Nucl. Phys. B206 (3): 333–348. Bibcode:1982NuPhB.206..333S. doi:10.1016/0550-3213(82)90271-1.
5. McGuire, Patrick C.; Steinhardt, Paul (May 2001). "Cracking open the window for strongly interacting massive particles as the halo dark matter". Proceedings of the 27th International Cosmic Ray Conference. 07-15 August. 4: 1566. arXiv:astro-ph/0105567. Bibcode:2001ICRC....4.1566M.
6. Tucker-Smith, David.; Weiner, Neal (February 2004). "The Status of inelastic dark matter". Physical Review D. 72 (6): 063509. arXiv:hep-ph/0402065. Bibcode:2005PhRvD..72f3509T. doi:10.1103/PhysRevD.72.063509. S2CID 115846489.
7. Servant, Geraldine.; Tait, Tim M.P. (September 2003). "Is the Lightest Kaluza–Klein Particle a Viable Dark Matter Candidate?". Nuclear Physics B. 650 (1–2): 391–419. arXiv:hep-ph/0206071. Bibcode:2003NuPhB.650..391S. doi:10.1016/S0550-3213(02)01012-X. S2CID 16222693.

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Hypothetical particles	Axino Axion Dark photon LSP Minicharged particle Neutralino Sterile neutrino SIMP WIMP WISP
Theories and objects	Cuspy halo problem Dark fluid Dark galaxy Dark globular cluster Dark matter halo Dark radiation Dark star Dwarf galaxy problem Halo mass function Mass dimension one fermions Massive compact halo object Mirror matter Navarro–Frenk–White profile Scalar field dark matter
Search experiments	Direct detection ADMX ANAIS ArDM CDEX CDMS CLEAN CoGeNT COSINE COSINUS COUPP CRESST CUORE D3 DAMA/LIBRA DAMA/NaI DAMIC DarkSide DARWIN DEAP DM-Ice DMTPC DRIFT EDELWEISS EURECA KIMS LUX LZ MACRO MIMAC NAIAD NEWAGE NEWS-G PandaX PICASSO PICO ROSEBUD SABRE SIMPLE TREX-DM UKDMC WARP XENON XMASS ZEPLIN Indirect detection AMS-02 ANTARES ATIC CALET CAST DAMPE Fermi HAWC HESS IceCube MAGIC MOA OGLE PAMELA VERITAS Other projects MultiDark PVLAS
Potential dark galaxies	HE0450-2958 HVC 127-41-330 Smith's Cloud VIRGOHI21
Related	Antimatter Dark energy Exotic matter Galaxy formation and evolution Illustris project Imaginary mass Negative mass UniverseMachine
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