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Warm dark matter

October 19, 2023

Warm dark matter (WDM) is a hypothesized form of dark matter that has properties intermediate between those of hot dark matter and cold dark matter, causing structure formation to occur bottom-up from above their free-streaming scale, and top-down below their free streaming scale. The most common WDM candidates are sterile neutrinos and gravitinos. The WIMPs (weakly interacting massive particles), when produced non-thermally, could be candidates for warm dark matter. In general, however, the thermally produced WIMPs are cold dark matter candidates.

keVins and GeVins Edit

One possible WDM candidate particle with a mass of a few keV comes from introducing two new, zero charge, zero lepton number fermions to the Standard Model of Particle Physics: "keV-mass inert fermions" (keVins) and "GeV-mass inert fermions" (GeVins). keVins are overproduced if they reach thermal equilibrium in the early universe, but in some scenarios the entropy production from the decays of unstable heavier particles may suppress their abundance to the correct value. These particles are considered "inert" because they only have suppressed interactions with the Z boson. Sterile neutrinos with masses of a few keV are possible candidates for keVins. At temperatures below the electroweak scale their only interactions with standard model particles are weak interactions due to their mixing with ordinary neutrinos. Due to the smallness of the mixing angle they are not overproduced because they freeze out before reaching thermal equilibrium. Their properties are consistent with astrophysical bounds coming from structure formation and the Pauli principle if their mass is larger than 1-8 keV.

In February 2014, different analyses[1][2] have extracted from the spectrum of X-ray emissions observed by XMM-Newton, a monochromatic signal around 3.5 keV. This signal is coming from different galaxy clusters (like Perseus and Centaurus) and several scenarios of warm dark matter can justify such a line. We can cite, for example, a 3.5 keV candidate annihilating into 2 photons,[3] or a 7 keV dark matter particle decaying into a photon and a neutrino.[4]

In November 2019, analysis of the interaction of various galactic halo matter on densities and distribution of stellar streams, coming off the satellites of the Milky Way, they were able to constrain minimums of mass for density perturbations by warm dark matter keVins in the GD-1 and Pal 5 streams. This lower limit on the mass of warm dark matter thermal relics mWDM > 4.6 keV; or adding dwarf satellite counts mWDM > 6.3 keV [5]

See also Edit

References Edit

  1. ^ Bulbul, Esra; Markevitch, Maxim; Foster, Adam; Smith, Randall K.; Loewenstein, Michael; Randall, Scott W. (2014-06-10). "Detection of an Unidentified Emission Line in the Stacked X-Ray Spectrum of Galaxy Clusters". The Astrophysical Journal. 789 (1): 13. arXiv:1402.2301. Bibcode:2014ApJ...789...13B. doi:10.1088/0004-637x/789/1/13. ISSN 0004-637X.
  2. ^ Boyarsky, A.; Ruchayskiy, O.; Iakubovskyi, D.; Franse, J. (2014-12-15). "Unidentified Line in X-Ray Spectra of the Andromeda Galaxy and Perseus Galaxy Cluster". Physical Review Letters. 113 (25): 251301. arXiv:1402.4119. Bibcode:2014PhRvL.113y1301B. doi:10.1103/physrevlett.113.251301. ISSN 0031-9007. PMID 25554871. S2CID 21406370.
  3. ^ Dudas, Emilian; Heurtier, Lucien; Mambrini, Yann (2014-08-04). "Generating x-ray lines from annihilating dark matter". Physical Review D. 90 (3): 035002. arXiv:1404.1927. Bibcode:2014PhRvD..90c5002D. doi:10.1103/physrevd.90.035002. ISSN 1550-7998. S2CID 118573978.
  4. ^ Ishida, Hiroyuki; Jeong, Kwang Sik; Takahashi, Fuminobu (2014). "7 keV sterile neutrino dark matter from split flavor mechanism". Physics Letters B. 732: 196–200. arXiv:1402.5837. Bibcode:2014PhLB..732..196I. doi:10.1016/j.physletb.2014.03.044. ISSN 0370-2693. S2CID 119226364.
  5. ^ Banik, Nilianjan; Bovy, Jo; Bertone, Gianfranco; Erkal, Denis; de Boer, T.J.L (2021). "Novel constraints on the particle nature of dark matter from stellar streams". Journal of Cosmology and Astroparticle Physics. 2021 (10): 043. arXiv:1911.02663. doi:10.1088/1475-7516/2021/10/043. S2CID 207847306.
  • Viel, Matteo; Lesgourgues, Julien; Haehnelt, Martin G.; Matarrese, Sabino; Riotto, Antonio (2005-03-31). "Constraining warm dark matter candidates including sterile neutrinos and light gravitinos with WMAP and the Lyman-αforest". Physical Review D. 71 (6): 063434. arXiv:astro-ph/0501562. Bibcode:2005PhRvD..71f3534V. doi:10.1103/physrevd.71.063534. ISSN 1550-7998. S2CID 119445620.
  • King, Stephen F; Merle, Alexander (2012-08-16). "Warm Dark Matter from keVins". Journal of Cosmology and Astroparticle Physics. 2012 (8): 016. arXiv:1205.0551. Bibcode:2012JCAP...08..016K. doi:10.1088/1475-7516/2012/08/016. ISSN 1475-7516. S2CID 118342558.
  • Gao, L.; Theuns, T. (2007-09-14). "Lighting the Universe with Filaments". Science. 317 (5844): 1527–1530. arXiv:0709.2165. Bibcode:2007Sci...317.1527G. doi:10.1126/science.1146676. ISSN 0036-8075. PMID 17872439. S2CID 18545632.
  • Lin, W. B.; Huang, D. H.; Zhang, X.; Brandenberger, R. (2001-02-05). "Nonthermal Production of Weakly Interacting Massive Particles and the Subgalactic Structure of the Universe". Physical Review Letters. 86 (6): 954–957. arXiv:astro-ph/0009003. Bibcode:2001PhRvL..86..954L. doi:10.1103/physrevlett.86.954. ISSN 0031-9007. PMID 11177983.
  • Millis, John. Warm Dark Matter. About.com. Retrieved 23 Jan., 2013. http://space.about.com/od/astronomydictionary/g/Warm-Dark-Matter.htm.

Further reading Edit


 

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October 19, 2023
warm, dark, matter, hypothesized, form, dark, matter, that, properties, intermediate, between, those, dark, matter, cold, dark, matter, causing, structure, formation, occur, bottom, from, above, their, free, streaming, scale, down, below, their, free, streamin. Warm dark matter WDM is a hypothesized form of dark matter that has properties intermediate between those of hot dark matter and cold dark matter causing structure formation to occur bottom up from above their free streaming scale and top down below their free streaming scale The most common WDM candidates are sterile neutrinos and gravitinos The WIMPs weakly interacting massive particles when produced non thermally could be candidates for warm dark matter In general however the thermally produced WIMPs are cold dark matter candidates Contents 1 keVins and GeVins 2 See also 3 References 4 Further readingkeVins and GeVins EditOne possible WDM candidate particle with a mass of a few keV comes from introducing two new zero charge zero lepton number fermions to the Standard Model of Particle Physics keV mass inert fermions keVins and GeV mass inert fermions GeVins keVins are overproduced if they reach thermal equilibrium in the early universe but in some scenarios the entropy production from the decays of unstable heavier particles may suppress their abundance to the correct value These particles are considered inert because they only have suppressed interactions with the Z boson Sterile neutrinos with masses of a few keV are possible candidates for keVins At temperatures below the electroweak scale their only interactions with standard model particles are weak interactions due to their mixing with ordinary neutrinos Due to the smallness of the mixing angle they are not overproduced because they freeze out before reaching thermal equilibrium Their properties are consistent with astrophysical bounds coming from structure formation and the Pauli principle if their mass is larger than 1 8 keV In February 2014 different analyses 1 2 have extracted from the spectrum of X ray emissions observed by XMM Newton a monochromatic signal around 3 5 keV This signal is coming from different galaxy clusters like Perseus and Centaurus and several scenarios of warm dark matter can justify such a line We can cite for example a 3 5 keV candidate annihilating into 2 photons 3 or a 7 keV dark matter particle decaying into a photon and a neutrino 4 In November 2019 analysis of the interaction of various galactic halo matter on densities and distribution of stellar streams coming off the satellites of the Milky Way they were able to constrain minimums of mass for density perturbations by warm dark matter keVins in the GD 1 and Pal 5 streams This lower limit on the mass of warm dark matter thermal relics mWDM gt 4 6 keV or adding dwarf satellite counts mWDM gt 6 3 keV 5 See also EditDark matter Hypothetical form of matter Hot dark matter HDM Theoretical form of dark matter particles which travel near the speed of light Cold dark matter CDM Hypothetical type of dark matter in physics Lambda CDM model Model of Big Bang cosmology Modified Newtonian dynamics Hypothesis proposing a modification of Newton s lawsReferences Edit Bulbul Esra Markevitch Maxim Foster Adam Smith Randall K Loewenstein Michael Randall Scott W 2014 06 10 Detection of an Unidentified Emission Line in the Stacked X Ray Spectrum of Galaxy Clusters The Astrophysical Journal 789 1 13 arXiv 1402 2301 Bibcode 2014ApJ 789 13B doi 10 1088 0004 637x 789 1 13 ISSN 0004 637X Boyarsky A Ruchayskiy O Iakubovskyi D Franse J 2014 12 15 Unidentified Line in X Ray Spectra of the Andromeda Galaxy and Perseus Galaxy Cluster Physical Review Letters 113 25 251301 arXiv 1402 4119 Bibcode 2014PhRvL 113y1301B doi 10 1103 physrevlett 113 251301 ISSN 0031 9007 PMID 25554871 S2CID 21406370 Dudas Emilian Heurtier Lucien Mambrini Yann 2014 08 04 Generating x ray lines from annihilating dark matter Physical Review D 90 3 035002 arXiv 1404 1927 Bibcode 2014PhRvD 90c5002D doi 10 1103 physrevd 90 035002 ISSN 1550 7998 S2CID 118573978 Ishida Hiroyuki Jeong Kwang Sik Takahashi Fuminobu 2014 7 keV sterile neutrino dark matter from split flavor mechanism Physics Letters B 732 196 200 arXiv 1402 5837 Bibcode 2014PhLB 732 196I doi 10 1016 j physletb 2014 03 044 ISSN 0370 2693 S2CID 119226364 Banik Nilianjan Bovy Jo Bertone Gianfranco Erkal Denis de Boer T J L 2021 Novel constraints on the particle nature of dark matter from stellar streams Journal of Cosmology and Astroparticle Physics 2021 10 043 arXiv 1911 02663 doi 10 1088 1475 7516 2021 10 043 S2CID 207847306 Viel Matteo Lesgourgues Julien Haehnelt Martin G Matarrese Sabino Riotto Antonio 2005 03 31 Constraining warm dark matter candidates including sterile neutrinos and light gravitinos with WMAP and the Lyman aforest Physical Review D 71 6 063434 arXiv astro ph 0501562 Bibcode 2005PhRvD 71f3534V doi 10 1103 physrevd 71 063534 ISSN 1550 7998 S2CID 119445620 King Stephen F Merle Alexander 2012 08 16 Warm Dark Matter from keVins Journal of Cosmology and Astroparticle Physics 2012 8 016 arXiv 1205 0551 Bibcode 2012JCAP 08 016K doi 10 1088 1475 7516 2012 08 016 ISSN 1475 7516 S2CID 118342558 Gao L Theuns T 2007 09 14 Lighting the Universe with Filaments Science 317 5844 1527 1530 arXiv 0709 2165 Bibcode 2007Sci 317 1527G doi 10 1126 science 1146676 ISSN 0036 8075 PMID 17872439 S2CID 18545632 Lin W B Huang D H Zhang X Brandenberger R 2001 02 05 Nonthermal Production of Weakly Interacting Massive Particles and the Subgalactic Structure of the Universe Physical Review Letters 86 6 954 957 arXiv astro ph 0009003 Bibcode 2001PhRvL 86 954L doi 10 1103 physrevlett 86 954 ISSN 0031 9007 PMID 11177983 Millis John Warm Dark Matter About com Retrieved 23 Jan 2013 http space about com od astronomydictionary g Warm Dark Matter htm Further reading EditBertone Gianfranco 2010 Particle Dark Matter Observations Models and Searches Cambridge University Press p 762 ISBN 978 0 521 76368 4 nbsp This physical cosmology related article is a stub You can help Wikipedia by expanding it vte nbsp This particle physics related article is a stub You can help Wikipedia by expanding it vte Retrieved from https en wikipedia org w index php title Warm dark matter amp oldid 1178049046, wikipedia, wiki, book, books, library,

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