The cuspy halo problem (also known as the core-cusp problem) is a discrepancy between the inferred dark matter density profiles of low-mass galaxies and the density profiles predicted by cosmological N-body simulations. Nearly all simulations form dark matter halos which have "cuspy" dark matter distributions, with density increasing steeply at small radii, while the rotation curves of most observed dwarf galaxies suggest that they have flat central dark matter density profiles ("cores").[1][2]
Several possible solutions to the core-cusp problem have been proposed. Many recent studies have shown that including baryonic feedback (particularly feedback from supernovae and active galactic nuclei) can "flatten out" the core of a galaxy's dark matter profile, since feedback-driven gas outflows produce a time-varying gravitational potential that transfers energy to the orbits of the collisionless dark matter particles.[3][4] Other works have shown that the core-cusp problem can be solved outside of the most widely accepted Cold Dark Matter (CDM) paradigm: simulations with warmorself-interacting dark matter also produce dark matter cores in low-mass galaxies.[5][6] It is also possible that the distribution of dark matter that minimizes the system energy has a flat central dark matter density profile.[7]
According to W.J.G. de Blok "The presence of a cusp in the centers of CDM halos is one of the earliest and strongest results derived from N-body cosmological simulations."[8] Numerical simulations for CDM structure formation predict some structure properties that conflict with astronomical observations.
The discrepancies range from galaxies to clusters of galaxies. "The main one that has attracted a lot of attention is the cuspy halo problem, namely that CDM models predict halos that have a high density core or have an inner profile that is too steep compared to observations."[9]
The conflict between numerical simulations and astronomical observations creates numerical constraints related to the core/cusp problem. Observational constraints on halo concentrations imply the existence of theoretical constraints on cosmological parameters. According to McGaugh, Barker, and de Blok,[10] there might be 3 basic possibilities for interpreting the halo concentration limits stated by them or anyone else:
One approach to solving the cusp-core problem in galactic halos is to consider models that modify the nature of dark matter; theorists have considered warm, fuzzy, self-interacting, and meta-cold dark matter, among other possibilities.[13] One straightforward solution could be that the distribution of dark matter that minimizes the system energy has a flat central dark matter density profile.[7]
{{cite journal}}: CS1 maint: multiple names: authors list (link)
{{cite journal}}: CS1 maint: multiple names: authors list (link)
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