Scalar Field Dark Matter
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In astrophysics Scalar Field Dark Matter is a classical minimally coupled real scalar field which has been postulated to account for the inferred dark matter.
The mass parameter of the scalar field is determined by the cut-off in the power spectrum at small scales, leading to a mass of about 
eV. [1]
The dark matter can be described as a Bose-Einstein condensate of the ultralight quanta of the field. The enormous Compton wavelength of these particles prevents structure formation on small subgalactic scales, which is a major problem in traditional cold dark matter models.
The collapse of initial overdensities is studied in Refs. [2]
[edit] References
- ^ V. Sahni and L. Wang, A New Cosmological Model of Quintessence and Dark Matter, Phys. Rev. D 62, 103517 (2000) preprint; T. Matos and L. A. Ureña-López, Quintessence and Scalar Dark Matter in the Universe, Class. Quant. Grav. 17, L75-L81 (2000) preprint; A Further Analysis of a Cosmological Model of Quintessence and Scalar Dark Matter, Phys. Rev. D 63, 063506 (2001) preprint.
- ^ M. Alcubierre, F. S. Guzmán, T. Matos, D. Núñez, L. A. Ureña-López and P. Wiederhold, Galactic Collapse of Scalar Field Dark Matter, Class. Quant. Grav. 19, 5017 (2002) preprint; F. S. Guzmán and L. A. Ureña-López, Evolution of the Schrödinger--Newton system for a self--gravitating scalar field, Phys. Rev. D 69, 124033 (2004) preprint; Gravitational cooling of self-gravitating Bose-Condensates, ApJ. 645, 814 (2006) preprint; A. Bernal and F. S. Guzmán, Scalar Field Dark Matter: non-spherical collapse and late time behavior, Phys. Rev. D 74, 063504 (2006) preprint.
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