Fuzzy cold dark matter is a hypothetical form of cold dark matter proposed to solve the cuspy halo problem. It would consist of extremely light scalar particles with masses on the order of eV; so a Compton wavelength on the order of 1 light year. Fuzzy cold dark matter halos in dwarf galaxies would manifest wave behavior on astrophysical scales, and the cusps would be avoided through the Heisenberg uncertainty principle. [1] The wave behavior leads to interference patterns, spherical soliton cores in dark matter halo centers, [2] and cylindrical soliton-like cores in dark matter cosmic web filaments. [3]
Fuzzy cold dark matter is a limit of scalar field dark matter without self-interaction. [4] [5] It is governed by the Schrödinger–Poisson equation.
New research (2023) has uncovered evidence that fuzzy dark matter, specifically ultralight axions, may better fit gravitational lens data than WIMP dark matter. [6]
Notes
- ^ Hu, Wayne; Barkana, Rennan; Gruzinov, Andrei (2000). "Cold and Fuzzy Dark Matter". Physical Review Letters. 85 (6): 1158–61. arXiv: astro-ph/0003365. Bibcode: 2000PhRvL..85.1158H. doi: 10.1103/PhysRevLett.85.1158. PMID 10991501. S2CID 118938504.
- ^ Schive, Hsi-Yu; Chiueh, Tzihong; Broadhurst, Tom (2014). "Cosmic structure as the quantum interference of a coherent dark wave". Nature Physics. 10 (7): 496–499. arXiv: 1406.6586. Bibcode: 2014NatPh..10..496S. doi: 10.1038/nphys2996. S2CID 118725080.
- ^ Mocz, Philip; Fialkov, Anastasia; Vogelsberger, Mark; Becerra, Fernando; Amin, Mustafa A.; Bose, Sownak; Boylan-Kolchin, Michael; Chavanis, Pierre-Henri; Hernquist, Lars; Lancaster, Lachlan; Marinacci, Federico; Robles, Victor H.; Zavala, Jesús (2019). "First Star-Forming Structures in Fuzzy Cosmic Filaments". Physical Review Letters. 123 (14): 141301. arXiv: 1910.01653. Bibcode: 2019PhRvL.123n1301M. doi: 10.1103/PhysRevLett.123.141301. ISSN 0031-9007. PMID 31702225. S2CID 203734641.
- ^ Bohua Li; Tanja Rindler-Daller; Paul R. Shapiro (2014). "Cosmological Constraints on Bose-Einstein-Condensed Scalar Field Dark Matter". Phys. Rev. D. 89 (8): 083536. arXiv: 1310.6061. Bibcode: 2014PhRvD..89h3536L. doi: 10.1103/PhysRevD.89.083536. S2CID 118654592.
- ^ Lee, Jae-Weon (2018). "Brief History of Ultra-light Scalar Dark Matter Models". EPJ Web of Conferences. 168: 06005. arXiv: 1704.05057. Bibcode: 2018EPJWC.16806005L. doi: 10.1051/epjconf/201816806005. S2CID 54649264.
- ^ Timmer, John (2023-04-21). "No WIMPS! Heavy particles don't explain gravitational lensing oddities". Ars Technica. Retrieved 2023-06-08.
 | This particle physics–related article is a stub. You can help Wikipedia by expanding it. |
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Fuzzy cold dark matter is a hypothetical form of cold dark matter proposed to solve the cuspy halo problem. It would consist of extremely light scalar particles with masses on the order of eV; so a Compton wavelength on the order of 1 light year. Fuzzy cold dark matter halos in dwarf galaxies would manifest wave behavior on astrophysical scales, and the cusps would be avoided through the Heisenberg uncertainty principle. [1] The wave behavior leads to interference patterns, spherical soliton cores in dark matter halo centers, [2] and cylindrical soliton-like cores in dark matter cosmic web filaments. [3]
Fuzzy cold dark matter is a limit of scalar field dark matter without self-interaction. [4] [5] It is governed by the Schrödinger–Poisson equation.
New research (2023) has uncovered evidence that fuzzy dark matter, specifically ultralight axions, may better fit gravitational lens data than WIMP dark matter. [6]
Notes
- ^ Hu, Wayne; Barkana, Rennan; Gruzinov, Andrei (2000). "Cold and Fuzzy Dark Matter". Physical Review Letters. 85 (6): 1158–61. arXiv: astro-ph/0003365. Bibcode: 2000PhRvL..85.1158H. doi: 10.1103/PhysRevLett.85.1158. PMID 10991501. S2CID 118938504.
- ^ Schive, Hsi-Yu; Chiueh, Tzihong; Broadhurst, Tom (2014). "Cosmic structure as the quantum interference of a coherent dark wave". Nature Physics. 10 (7): 496–499. arXiv: 1406.6586. Bibcode: 2014NatPh..10..496S. doi: 10.1038/nphys2996. S2CID 118725080.
- ^ Mocz, Philip; Fialkov, Anastasia; Vogelsberger, Mark; Becerra, Fernando; Amin, Mustafa A.; Bose, Sownak; Boylan-Kolchin, Michael; Chavanis, Pierre-Henri; Hernquist, Lars; Lancaster, Lachlan; Marinacci, Federico; Robles, Victor H.; Zavala, Jesús (2019). "First Star-Forming Structures in Fuzzy Cosmic Filaments". Physical Review Letters. 123 (14): 141301. arXiv: 1910.01653. Bibcode: 2019PhRvL.123n1301M. doi: 10.1103/PhysRevLett.123.141301. ISSN 0031-9007. PMID 31702225. S2CID 203734641.
- ^ Bohua Li; Tanja Rindler-Daller; Paul R. Shapiro (2014). "Cosmological Constraints on Bose-Einstein-Condensed Scalar Field Dark Matter". Phys. Rev. D. 89 (8): 083536. arXiv: 1310.6061. Bibcode: 2014PhRvD..89h3536L. doi: 10.1103/PhysRevD.89.083536. S2CID 118654592.
- ^ Lee, Jae-Weon (2018). "Brief History of Ultra-light Scalar Dark Matter Models". EPJ Web of Conferences. 168: 06005. arXiv: 1704.05057. Bibcode: 2018EPJWC.16806005L. doi: 10.1051/epjconf/201816806005. S2CID 54649264.
- ^ Timmer, John (2023-04-21). "No WIMPS! Heavy particles don't explain gravitational lensing oddities". Ars Technica. Retrieved 2023-06-08.
|
| This particle physics–related article is a stub. You can help Wikipedia by expanding it. |
|
| This physical cosmology-related article is a stub. You can help Wikipedia by expanding it. |