Scalar field dark matter
The universe may be accelerating, fueled perhaps by a cosmological constant or some other field possessing long range ‘repulsive’ effects. A model must predict the correct form for the large scale clustering spectrum, account for cosmic microwave background anisotropies on large and intermediate angular scales, and provide agreement with the luminosity distance relation obtained from observations of high redshift supernovae. The modeled evolution of the universe includes a large amount of unknown matter and energy in order to agree with such observations. This energy density has two components: cold dark matter and dark energy. Each contributes to the theory of the origination of galaxies and the expansion of the universe. The universe must have a critical density, a density not explained by baryonic matter (ordinary matter) alone.
The dark matter can be modeled as a scalar field using two fitted parameters, mass and self-interaction. In this picture the dark matter consists of an ultralight particle with a mass of ~10−22 eV when there is no self-interaction. If there is a self-interaction a wider mass range is allowed. The uncertainty in position of a particle is larger than its Compton wavelength, and for some reasonable estimates of particle mass and density of dark matter there is no point talking about the individual particle's position and momentum. The dark matter is more like a wave than a particle, and the galactic halos are giant systems of condensed bose liquid, possibly superfluid. The dark matter can be described as a Bose–Einstein condensate of the ultralight quanta of the field and as boson stars. 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.
This dark matter model is also known as BEC dark matter or wave dark matter. Fuzzy dark matter and ultra-light axion are examples of scalar field dark matter.
- Weakly interacting massive particles – Hypothetical particles that are thought to constitute dark matter
- Minimal Supersymmetric Standard Model
- Dark matter halo – A theoretical component of a galaxy that envelops the galactic disc and extends well beyond the edge of the visible galaxy
- Light dark matter – Dark matter weakly interacting massive particles candidates with masses less than 1 GeV
- Hot dark matter – A theoretical form of dark matter which consists of particles that travel with ultrarelativistic velocities
- Warm dark matter – A hypothesized form of dark matter that has properties intermediate between those of hot dark matter and cold dark matter
- Fuzzy cold dark matter – A hypothetical form of cold dark matter proposed to solve the cuspy halo problem
- Jeremiah P. Ostriker and Paul Steinhardt New Light on Dark Matter
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- Galaxies are not scattered about the universe in a random way, but rather form an intricate network of filaments, sheets, and clusters. How these large-scale structures formed is at the root of many key questions in cosmology.
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