Fuzzy cold dark matter

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.

Notes
  1. 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.
  2. Schive, Hsi-Yu; Chiueh, Tzihong; Broadhurst, Tom (2014). "Cosmic structure as the quantum interference of a coherent dark wave". Nature Physics. 10: 496499. arXiv:1406.6586. doi:10.1038/nphys2996.
  3. 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.
  4. 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.
  5. 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.


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