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Self-interacting dark matter

From Wikipedia, the free encyclopedia
Hypothetical form of dark matter

Inastrophysics andparticle physics,self-interacting dark matter (SIDM) is an alternative class ofdark matter particles that have strong interactions, in contrast to the standardcold dark matter model (CDM). SIDM was postulated in 2000[1] as a solution to thecore-cusp problem.[2][3][4] In the simplest models of DM self-interactions, a Yukawa-type potential and a force carrierφ mediates between two dark matter particles.[5] On galactic scales, DM self-interaction leads to energy and momentum exchange between DM particles. Over cosmological time scales this results in isothermal cores in the central region of dark matter haloes.

If the self-interacting dark matter is inhydrostatic equilibrium, its pressure and density follow:

Pχ/ρχ=Φtot=(Φχ+Φb),{\displaystyle \nabla P_{\chi }/\rho _{\chi }=\nabla \Phi _{\text{tot}}=\nabla (\Phi _{\chi }+\Phi _{\text{b}}),}

whereΦχ{\displaystyle \Phi _{\chi }} andΦb{\displaystyle \Phi _{\text{b}}} are the gravitational potential of the dark matter and a baryon respectively. The equation naturally correlates the dark matter distribution to that of the baryonic matter distribution. With this correlation, the self-interacting dark matter can explain phenomena such as theTully–Fisher relation.

Self-interacting dark matter has also been postulated as an explanation for theDAMA annual modulation signal.[6][7][8] Moreover, it is shown that it can serve the seed ofsupermassive black holes at high redshift.[9] SIDM may have originated in a so-called "Dark Big Bang".[10]

In July 2024 a study proposed SIDM solves the "final-parsec problem",[11][12] two months later another study proposed the same withfuzzy cold dark matter.[13][14]

See also

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References

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  1. ^Spergel, David N.; Steinhardt, Paul J. (April 2000)."Observational Evidence for Self-Interacting Cold Dark Matter".Physical Review Letters.84 (17):3760–3763.arXiv:astro-ph/9909386.Bibcode:2000PhRvL..84.3760S.doi:10.1103/PhysRevLett.84.3760.ISSN 0031-9007.PMID 11019199.S2CID 6669358.
  2. ^Moore, Ben (August 1994)."Evidence against dissipation-less dark matter from observations of galaxy haloes".Nature.370 (6491):629–631.Bibcode:1994Natur.370..629M.doi:10.1038/370629a0.ISSN 0028-0836.S2CID 4325561.
  3. ^Oh, Se-Heon; de Blok, W. J. G.; Walter, Fabian; Brinks, Elias; Kennicutt, Robert C. (December 2008)."High-Resolution Dark Matter Density Profiles of THINGS Dwarf Galaxies: Correcting for Noncircular Motions".The Astronomical Journal.136 (6):2761–2781.arXiv:0810.2119.Bibcode:2008AJ....136.2761O.doi:10.1088/0004-6256/136/6/2761.ISSN 0004-6256.
  4. ^Oh, Se-Heon; Hunter, Deidre A.; Brinks, Elias; Elmegreen, Bruce G.; Schruba, Andreas; Walter, Fabian; Rupen, Michael P.; Young, Lisa M.; Simpson, Caroline E.; Johnson, Megan C.; Herrmann, Kimberly A. (June 2015)."High-resolution Mass Models of Dwarf Galaxies from LITTLE THINGS".The Astronomical Journal.149 (6): 180.arXiv:1502.01281.Bibcode:2015AJ....149..180O.doi:10.1088/0004-6256/149/6/180.ISSN 0004-6256.
  5. ^Loeb, Abraham; Weiner, Neal (April 2011)."Cores in Dwarf Galaxies from Dark Matter with a Yukawa Potential".Physical Review Letters.106 (17) 171302.arXiv:1011.6374.Bibcode:2011PhRvL.106q1302L.doi:10.1103/PhysRevLett.106.171302.ISSN 0031-9007.PMID 21635025.
  6. ^Mitra, Saibal (15 June 2005). "Has DAMA detected self-interacting dark matter?".Physical Review D.71 (12) 121302.arXiv:astro-ph/0409121.Bibcode:2005PhRvD..71l1302M.doi:10.1103/PhysRevD.71.121302.S2CID 31554326.
  7. ^Moskowitz, Clara (20 April 2015)."Dark Matter May Feel a "Dark Force" That the Rest of the Universe Does Not".Scientific American.
  8. ^Richard Massey; et al. (June 2015)."The behaviour of dark matter associated with four bright cluster galaxies in the 10 kpc core of Abell 3827".Monthly Notices of the Royal Astronomical Society.449 (4P):3393–3406.arXiv:1504.03388.Bibcode:2015MNRAS.449.3393M.doi:10.1093/mnras/stv467. commentaryThe Possible First Signs of Self-interacting Dark Matter
  9. ^Feng, W.-X.; Yu, H.-B.; Zhong, Y.-M. (2021)."Seeding Supermassive Black Holes with Self-interacting Dark Matter: A Unified Scenario with Baryons".The Astrophysical Journal Letters.914 (2): L26.arXiv:2010.15132.Bibcode:2021ApJ...914L..26F.doi:10.3847/2041-8213/ac04b0."How a supermassive black hole originates: Study points to a seed black hole produced by a dark matter halo collapse."ScienceDaily, 16 June 2021.
  10. ^"Dancing in the dark".The Economist. 9 March 2024.
  11. ^Alonso-Álvarez, Gonzalo; Cline, James M.; Dewar, Caitlyn (2024-07-09)."Self-Interacting Dark Matter Solves the Final Parsec Problem of Supermassive Black Hole Mergers".Physical Review Letters.133 (2) 021401.arXiv:2401.14450.Bibcode:2024PhRvL.133b1401A.doi:10.1103/PhysRevLett.133.021401.ISSN 0031-9007.PMID 39073950.
  12. ^Jonathan Gilbert (2024-08-19)."'Final parsec problem' that makes supermassive black holes impossible to explain could finally have a solution".livescience.com. Retrieved2024-08-20.
  13. ^Koo, Hyeonmo; Bak, Dongsu; Park, Inkyu; Hong, Sungwook E.; Lee, Jae-Weon (September 2024)."Final parsec problem of black hole mergers and ultralight dark matter".Physics Letters B.856 138908.arXiv:2311.03412.Bibcode:2024PhLB..85638908K.doi:10.1016/j.physletb.2024.138908.
  14. ^O'Callaghan, Jonathan (2024-10-23)."How Do Merging Supermassive Black Holes Pass the Final Parsec?".Quanta Magazine. Retrieved2024-10-24.

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