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Strongly interacting massive particle

In this article, the impact of Strongly interacting massive particle on contemporary society will be addressed, analyzing its economic, social and cultural implications. Strongly interacting massive particle has become a topic of interest for academics, professionals and the general public, due to its relevance in today's world. Throughout the next sections, the evolution of Strongly interacting massive particle over time, as well as its influence on different aspects of daily life, will be explored. Likewise, the various opinions and positions on Strongly interacting massive particle will be examined, with the aim of offering a comprehensive and plural vision of this phenomenon.

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A strongly interacting massive particle (SIMP) is a hypothetical particle that interacts strongly between themselves and weakly with ordinary matter, but could form the inferred dark matter despite this.[1][2][3]

Strongly interacting massive particles have been proposed as a solution for the ultra-high-energy cosmic-ray problem[4][5] and the absence of cooling flows in galactic clusters.[6][7]

Various experiments and observations have set constraints on SIMP dark matter from 1990 onward.[8][9][10][11][12][13]

SIMP annihilations would produce significant heat. DAMA set limits with NaI(Tl) crystals.[11][citation needed]

Measurements of Uranus's heat excess exclude SIMPs from 150 MeV to 104 GeV.[14] Earth's heat flow significantly constrains any cross section.[15]

See also

References

  1. ^ Wandelt, Benjamin D; Dave, Romeel; Farrar, Glennys R; McGuire, Patrick C; Spergel, David N; Steinhardt, Paul J (2000), "Self-Interacting Dark Matter", in Cline, David B (ed.), Sources and Detection of Dark Matter and Dark Energy in the Universe, Springer-Verlag, p. 263, arXiv:astro-ph/0006344, Bibcode:2001sddm.symp..263W, ISBN 978-3-540-41216-8
  2. ^ Massey, Richard; et al. (2017), "Dark matter dynamics in Abell 3827: new data consistent with standard Cold Dark Matter", Monthly Notices of the Royal Astronomical Society, 477 (1): 669–677, arXiv:1708.04245, Bibcode:2018MNRAS.477..669M, doi:10.1093/mnras/sty630
  3. ^ Grossman, Lisa (April 5, 2018). "Dark matter isn't interacting with itself after all". ScienceNews. Archived from the original on 2018-04-06. Retrieved 2018-04-05.
  4. ^ Chung, Daniel J. H; Farrar, Glennys R; Kolb, Edward W (1998), "Are ultrahigh energy cosmic rays signals of supersymmetry?", Physical Review D, 57 (8): 4606, arXiv:astro-ph/9707036, Bibcode:1998PhRvD..57.4606C, doi:10.1103/PhysRevD.57.4606, S2CID 44780458
  5. ^ Albuquerque, Ivone F. M; Farrar, Glennys R; Kolb, Edward W (1998), "Exotic massive hadrons and ultra-high energy cosmic rays", Physical Review D, 59 (1) 015021, arXiv:hep-ph/9805288, Bibcode:1998PhRvD..59a5021A, doi:10.1103/PhysRevD.59.015021
  6. ^ Qin, Bo; Wu, Xiang-Ping (2001), "Constraints on the Interaction between Dark Matter and Baryons from Cooling Flow Clusters", Physical Review Letters, 87 (6) 061301, arXiv:astro-ph/0106458, Bibcode:2001PhRvL..87f1301Q, doi:10.1103/PhysRevLett.87.061301, PMID 11497819, S2CID 13510283
  7. ^ Chuzhoy, Leonid; Nusser, Adi (2006), "Consequences of short range interactions between dark matter and protons in galaxy clusters", The Astrophysical Journal, 645 (2): 950–954, arXiv:astro-ph/0408184, Bibcode:2006ApJ...645..950C, doi:10.1086/504505, S2CID 16131656
  8. ^ Starkman, Glenn D; Gould, Andrew; Esmailzadeh, Rahim; Dimopoulos, Savas (1990), "Opening the window on strongly interacting dark matter", Physical Review D, 41 (12): 3594–3603, Bibcode:1990PhRvD..41.3594S, doi:10.1103/PhysRevD.41.3594, PMID 10012303
  9. ^ Cyburt, Richard H; Fields, Brian D; Pavlidou, Vasiliki; Wandelt, Benjamin D (2002), "Constraining Strong Baryon-Dark Matter Interactions with Primordial Nucleosynthesis and Cosmic Rays", Physical Review D, 65 (12) 123503, arXiv:astro-ph/0203240, Bibcode:2002PhRvD..65l3503C, doi:10.1103/PhysRevD.65.123503, S2CID 14926247.
  10. ^ Zaharijas, Gabrijela; Farrar, Glennys R (2004), "A Window in the Dark Matter Exclusion Limits", Physical Review D, 72 (8) 083502, arXiv:astro-ph/0406531, Bibcode:2005PhRvD..72h3502Z, doi:10.1103/PhysRevD.72.083502, S2CID 39245145
  11. ^ a b Bacci, C.; et al. (1996), "Improved limits on strongly interacting massive particles with NaI(Tl) scintillators", Astroparticle Physics, 4 (3): 195–198, Bibcode:1996APh.....4..195B, doi:10.1016/0927-6505(95)00032-1
  12. ^ McGuire, Patrick C; Steinhardt, Paul J (2001), "Cracking Open the Window for Strongly Interacting Massive Particles as the Halo Dark Matter", Proceedings of the International Cosmic Ray Conference, vol. 4, Hamburg, Germany, p. 1566, arXiv:astro-ph/0105567, Bibcode:2001ICRC....4.1566M{{cite book}}: CS1 maint: location missing publisher (link)
  13. ^ Javorsek II, D; Fischbach, E; Teplitz, V (2002), "New Experimental Bounds on the Contributions to the Cosmological Density Parameter Ω from Strongly Interacting Massive Particles", The Astrophysical Journal, 568 (1): 1–8, Bibcode:2002ApJ...568....1J, doi:10.1086/338796
  14. ^ Mitra, Saibal (2004), "Uranus's anomalously low excess heat constrains strongly interacting dark matter", Physical Review D, 70 (10) 103517, arXiv:astro-ph/0408341, Bibcode:2004PhRvD..70j3517M, doi:10.1103/PhysRevD.70.103517, S2CID 53396770
  15. ^ Mack, Gregory D; Beacom, John F; Bertone, Gianfranco (2007), "Towards Closing the Window on Strongly Interacting Dark Matter: Far-Reaching Constraints from Earth's Heat Flow", Physical Review D, 76 (4) 043523, arXiv:0705.4298, Bibcode:2007PhRvD..76d3523M, doi:10.1103/PhysRevD.76.043523, S2CID 119710504

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