Strongly interacting massive particle

{{Short description|Hypothetical particle}}

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.

{{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

}}

{{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

}}{{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

}}

Strongly interacting massive particles have been proposed as a solution for the ultra-high-energy cosmic-ray problem

{{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

}}

{{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

}} and the absence of cooling flows in galactic clusters.

{{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

}}

{{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

}}

Various experiments and observations have set constraints on SIMP dark matter from 1990 onward.

{{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

}}

{{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

}}.

{{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

}}

{{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

}}

{{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}}

{{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

}}

SIMP annihilations would produce significant heat. DAMA set limits with NaI(Tl) crystals.{{citation needed|date=January 2017}}

Measurements of Uranus's heat excess exclude SIMPs from 150 MeV to 10⁴ GeV.

{{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

}} Earth's heat flow significantly constrains any cross section.

{{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

}}