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{{short description|Hypothetical particles that interact strongly with ordinary matter, but could form the inferred dark matter despite this}}
{{For|the brown dwarf or exoplanet|SIMP J013656.5+093347}}
'''Strongly interacting massive particles''' ('''SIMPs''') are hypothetical particles that [[strong interaction|interact strongly]] between themselves [looks like they scatter off each other - observation of colliding galaxies in the [[Abell 3827]] cluster, where it seemed that dark matter lagged behind the ordinary matter] and weakly with ordinary matter, but could form the inferred [[dark matter]] despite this.<ref name="wand">
{{cite book
|last1=Wandelt |first1=Benjamin D
|last2=Dave |first2=Romeel
|last3=Farrar |first3=Glennys R
|last4=McGuire |first4=Patrick C
|last5=Spergel |first5=David N
|last6=Steinhardt |first6=Paul J
|year=2000
|chapter=Self-Interacting Dark Matter
|title=Sources and Detection of Dark Matter and Dark Energy in the Universe
|journal=<!-- -->
|editor-last=Cline |editor-first=David B
|publisher=Springer-Verlag
|pages=263
|arxiv=astro-ph/0006344
|mode=cs2
|bibcode=2001sddm.symp..263W
|isbn=978-3-540-41216-8
}}</ref> However, this finding has since been discounted based on further observations and modelling of the cluster.<ref>
{{cite journal
|last1=Massey |first1=Richard
|display-authors=etal
|year=2017
|title=Dark matter dynamics in Abell 3827: new data consistent with standard Cold Dark Matter
|journal=Monthly Notices of the Royal Astronomical Society
|volume=477
|pages=669–677
|arxiv=1708.04245
|mode=cs2
|doi=10.1093/mnras/sty630
}}</ref><ref>
{{cite web
|last1=Grossman |first1=Lisa
|date=April 5, 2018
|title=Dark matter isn't interacting with itself after all
|url=https://www.sciencenews.org/article/dark-matter-isnt-interacting-itself-after-all
|work=ScienceNews
|accessdate=2018-04-05
}}</ref>
Strongly interacting massive particles have been proposed as a solution for the [[Ultra-high-energy cosmic ray|ultra-high-energy cosmic-ray]] problem<ref name="chung">
{{Cite journal
|last1=Chung |first1=Daniel J. H
|last2=Farrar |first2=Glennys R
|last3=Kolb |first3=Edward W
|year=1998
|title=Are ultrahigh energy cosmic rays signals of supersymmetry?
|journal=Physical Review D
|volume=57 |issue=8 |pages=4606
|arxiv=astro-ph/9707036
|bibcode=1998PhRvD..57.4606C
|doi=10.1103/PhysRevD.57.4606
|mode=cs2
}}</ref><ref name="albq">
{{Cite journal
|last1=Albuquerque |first1=Ivone F. M
|last2=Farrar |first2=Glennys R
|last3=Kolb |first3=Edward W
|year=1998
|title=Exotic massive hadrons and ultra-high energy cosmic rays
|journal=Physical Review D
|volume=59 |issue=1 |page=015021
|arxiv=hep-ph/9805288
|bibcode=1999PhRvD..59a5021A
|doi=10.1103/PhysRevD.59.015021
|mode=cs2
}}</ref> and the absence of [[Cooling flow|cooling flows in galactic clusters]].<ref name="qin">
{{Cite journal
|last1=Qin |first1=Bo
|last2=Wu |first2=Xiang-Ping
|year=2001
|title=Constraints on the Interaction between Dark Matter and Baryons from Cooling Flow Clusters
|journal=Physical Review Letters
|volume=87 |issue=6 |page=061301
|arxiv=astro-ph/0106458
|bibcode=2001PhRvL..87f1301Q
|doi=10.1103/PhysRevLett.87.061301
|pmid=11497819
|mode=cs2
}}</ref><ref name="chuz">
{{Cite journal
|last1=Chuzhoy |first1=Leonid
|last2=Nusser |first2=Adi
|year=2006
|title=Consequences of short range interactions between dark matter and protons in galaxy clusters
|journal=The Astrophysical Journal
|volume=645 |issue=2 |pages=950–954
|arxiv=astro-ph/0408184
|bibcode=2006ApJ...645..950C
|doi=10.1086/504505
|mode=cs2
}}</ref>
Various experiments and observations have set constraints on SIMP dark matter from 1990 onward.<ref name="stark">
{{cite journal
|last1=Starkman |first1=Glenn D
|last2=Gould |first2=Andrew
|last3=Esmailzadeh |first3=Rahim
|last4=Dimopoulos |first4=Savas
|year=1990
|title=Opening the window on strongly interacting dark matter
|journal=Physical Review D
|volume=41 |issue=12 |pages=3594
|bibcode=1990PhRvD..41.3594S
|doi=10.1103/PhysRevD.41.3594
|mode=cs2
|url=http://cds.cern.ch/record/212913
}}</ref><ref name="cyb">
{{Cite journal
|last1=Cyburt |first1=Richard H
|last2=Fields |first2=Brian D
|last3=Pavlidou |first3=Vasiliki
|last4=Wandelt |first4=Benjamin D
|year=2002
|title=Constraining Strong Baryon-Dark Matter Interactions with Primordial Nucleosynthesis and Cosmic Rays
|journal=Physical Review D
|volume=65 |issue=12 |page=123503
|arxiv=astro-ph/0203240
|bibcode=2002PhRvD..65l3503C
|doi=10.1103/PhysRevD.65.123503
|mode=cs2
}}.</ref><ref name="zahar">
{{Cite journal
|last1=Zaharijas |first1=Gabrijela
|last2=Farrar |first2=Glennys R
|year=2004
|title=A Window in the Dark Matter Exclusion Limits
|journal=Physical Review D
|volume=72 |issue=8 |page=083502
|arxiv=astro-ph/0406531
|bibcode=2005PhRvD..72h3502Z
|doi=10.1103/PhysRevD.72.083502
|mode=cs2
}}</ref><ref name="wdn">
{{cite journal
|last1=Bacci |first1=C.
|display-authors=etal
|year=1996
|title=Improved limits on strongly interacting massive particles with NaI(Tl) scintillators
|journal=Astroparticle Physics
|volume=4 |issue=3 |pages=195–198
|bibcode=1996APh.....4..195B
|doi=10.1016/0927-6505(95)00032-1
|mode=cs2
}}</ref><ref name="mcgr">
{{Cite book
|last1=McGuire |first1=Patrick C
|last2=Steinhardt |first2=Paul J
|year=2001
|chapter=Cracking Open the Window for Strongly Interacting Massive Particles as the Halo Dark Matter
|title=Proceedings of the International Cosmic Ray Conference
|journal=International Cosmic Ray Conference
|volume=4
|___location=Hamburg, Germany
|page=1566
|arxiv=astro-ph/0105567
|mode=cs2
|bibcode=2001ICRC....4.1566M}}</ref><ref name="javor">
{{cite journal
|last1=Javorsek II |first1=D
|last2=Fischbach |first2=E
|last3=Teplitz |first3=V
|year=2002
|title=New Experimental Bounds on the Contributions to the Cosmological Density Parameter Ω from Strongly Interacting Massive Particles
|journal=The Astrophysical Journal
|volume=568 |issue=1
|pages=1–8
|bibcode=2002ApJ...568....1J
|doi=10.1086/338796
|mode=cs2
}}</ref>
SIMPs annihilations would produce significant heat. [[DAMA/NaI|DAMA]] set limits with NaI(Tl) crystals.<ref name="wdn"/>{{citation needed|date=January 2017}}
Measurements of [[Uranus]]'s heat excess exclude SIMPS from 150 MeV to 10<sup>4</sup> GeV.<ref name="mitr">
{{Cite journal
|last1=Mitra |first1=Saibal
|year=2004
|title=Uranus's anomalously low excess heat constrains strongly interacting dark matter
|journal=Physical Review D
|volume=70 |issue=10 |page=103517
|arxiv=astro-ph/0408341
|bibcode=2004PhRvD..70j3517M
|doi=10.1103/PhysRevD.70.103517
|mode=cs2
}}</ref> Earth's heat flow significantly constrains any cross section.<ref>
{{Cite journal
|last1=Mack |first1=Gregory D
|last2=Beacom |first2=John F
|last3=Bertone |first3=Gianfranco
|year=2007
|title=Towards Closing the Window on Strongly Interacting Dark Matter: Far-Reaching Constraints from Earth's Heat Flow
|journal=Physical Review D
|volume=76 |issue=4 |page=043523
|arxiv=0705.4298
|bibcode=2007PhRvD..76d3523M
|doi=10.1103/PhysRevD.76.043523
|mode=cs2
}}</ref>
==See also==
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