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{{Short description|Hypothetical particle}}
In [[astrophysics]] '''SIMP''' is an abbreviation of '''Strongly Interacting Massive Particle'''. SIMPs could form the inferred [[dark matter]] despite their strong interactions with ordinary matter.<ref name="wand">B. D. Wandelt, R. Dave, G. R. Farrar, P. C. McGuire, D. N. Spergel and P. J. Steinhardt, ''Self-Interacting Dark Matter'', Marina del Rey 2000, Sources and detection of dark matter and dark energy in the universe, 263 (2000), [http://arxiv.org/abs/astro-ph/0006344 preprint].</ref>
A '''strongly interacting massive particle''' ('''SIMP''') is a hypothetical particle that [[strong interaction|interacts strongly]] between themselves and [[Weak interaction|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><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
|issue=1
|pages=669–677
|arxiv=1708.04245
|mode=cs2
|doi=10.1093/mnras/sty630
|doi-access=free
|bibcode=2018MNRAS.477..669M
}}</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
|access-date=2018-04-05
|archive-date=2018-04-06
|archive-url=https://web.archive.org/web/20180406013104/https://www.sciencenews.org/article/dark-matter-isnt-interacting-itself-after-all
|url-status=live
}}</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
|s2cid=44780458
|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=1998PhRvD..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
|s2cid=13510283
|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
|s2cid=16131656
|mode=cs2
}}</ref>
 
Various experiments and observations have set constraints on SIMP dark matter from 1990 onward.<ref name="stark">
SIMPs have been proposed as a solution for the ultra high energy cosmic ray problem<ref name="chung">D. Chung, G. R. Farrar and E. W. Kolb, ''Are ultrahigh energy cosmic rays signals of supersymmetry?'', Phys. Rev. D '''57''', 4606 (1998) [http://arxiv.org/abs/astro-ph/9707036 preprint].</ref><ref name="albq">I. F. M. Albuquerque, G. R. Farrar and E. W. Kolb, ''Exotic massive hadrons and ultra-high energy cosmic rays'', Phys. Rev. D '''59''', 015021 (1999) [http://arxiv.org/abs/hep-ph/9805288 preprint].</ref> and for the absence of cooling flows.<ref name="qin">B. Qin and X. P. Wu, ''Constraints on the Interaction between Dark Matter and Baryons from Cooling Flow Clusters'', Phys. Rev. Lett. '''87''', 061301 (2001) [http://arxiv.org/abs/astro-ph/0106458 preprint].</ref><ref name="chuz">L. Chuzhoi and A. Nusser, ''A limit on the dark matter and baryons interaction cross-section in galaxy clusters'', [http://arxiv.org/abs/astro-ph/0408184 preprint].</ref> Various experiments and observations have set constraints on SIMP dark matter.<ref name="wand"/><ref name="stark">G. D. Starkman, A. Gould, R. Esmailzadeh, and S. Dimopoulos, ''Opening the window on strongly interacting dark matter'', Phys. Rev. D '''41''', 3594 (1990).</ref><ref name="mcgr">P. C. McGuire and P. J. Steinhardt, ''Cracking Open the Window for Strongly Interacting Massive Particles as the Halo Dark Matter'', Proceedings of the International Cosmic Ray Conference, Hamburg, Germany, 1566 (2001), [http://arxiv.org/abs/astro-ph/0105567 preprint].</ref><ref name="cyb">R. H. Cyburt, B. D. Fields, V. Pavlidou and B. D. Wandelt, ''Constraining Strong Baryon-Dark Matter Interactions with Primordial Nucleosynthesis and Cosmic Rays'', Phys. Rev. D '''65''', 123503 (2002) [http://arxiv.org/abs/astro-ph/0203240 preprint].</ref><ref name="mitr">S. Mitra, ''Uranus's anomalously low excess heat constrains strongly interacting dark matter'', Phys. Rev. D '''70''', 103517 (2004) [http://arxiv.org/abs/astro-ph/0408341 preprint].</ref><ref>G. D. Mack, J. F. Beacom and G. Bertone, ''Towards Closing the Window on Strongly Interacting Dark Matter: Far-Reaching Constraints from Earth's Heat Flow'', Phys. Rev. D '''76''', 043523 (2007) [http://arxiv.org/abs/0705.4298 preprint].</ref><ref name="zahar">G. Zaharijas and G. R. Farrar, ''Window in the dark matter exclusion limits'', Phys. Rev. D '''72''', 083502 (2005) [http://arxiv.org/abs/astro-ph/0406531 preprint].</ref><ref name="javor">D. Javorsek II, E. Fischbach and V. Teplitz, ''New experimental bounds on the contributions to the cosmological density parameter <math>\Omega</math> from strongly interacting massive particles'', ApJ '''568''', 1 (2002).</ref>
{{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=3594–3603
|bibcode=1990PhRvD..41.3594S
|doi=10.1103/PhysRevD.41.3594
|pmid=10012303
|mode=cs2
|url=https://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| authorlink3=Vasiliki Pavlidou
|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
|s2cid=14926247
|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
|s2cid=39245145
|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
|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
|doi-access=free
}}</ref>
 
SIMP 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
|s2cid=53396770
|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
|s2cid=119710504
|mode=cs2
}}</ref>
 
==See also==
*{{annotated link|Weakly interacting massive particles}}
*[[WIMP|Weakly Interacting Massive Particles]]
*{{annotated link|Self-interacting dark matter}}
*{{annotated link|Massive compact halo object}}
 
==References==
{{Reflist}}
<div class="references-small">
 
<references/>
==Further reading==
</div>
*{{Cite book
| last = Bertone
| first = Gianfranco
| authorlink =
| title = Particle Dark Matter: Observations, Models and Searches
| publisher = [[Cambridge University Press]]
| year = 2010
| ___location =
| pages = 762
| url =
| doi =
| id =
| isbn = 978-0-521-76368-4| title-link = Particle Dark Matter
| bibcode = 2010pdmo.book.....B
}}
{{Dark matter}}
 
[[Category:Dark matter]]
[[Category:Astroparticle physics]]
[[Category:Hypothetical particles]]
 
{{particle-stub}}
 
Alternate definition for SIMP. Root words are pimp and sissy.
 
(1)-The common simp can be found with a girlfriend, so in a sense is a pimp but is a sissy for being with a cunniving female who does not want to be with him in the first place. Ex. Eric is a simp for being in love with a female that cheated on him but ignores the fact in hopes of maintaining his happy relationship.
 
(2)- A simp can also be found tagging behing large groups of females in hopes of achieving sexual intercourse. He will allow the females to play him to their advantage, all the while not caring. Ex. After countless nights of no success Travis continues to chase the females endlessly while not even caring he will never reach touchdown status.
 
Synonyms include but are not limited too: mark, trick, wimp, sucker, and sissy
Retrieved from "https://en.wikipedia.org/wiki/Strongly_interacting_massive_particle"