The Core-Cusp Problem

By W. J. Blok. 2009

711 citations recorded by the source corpus.

This paper gives an overview of the attempts to determine the distribution of dark matter in low surface brightness disk and gas-rich dwarf galaxies, both through observations and computer simulations. Observations seem to indicate an approximately constant dark matter density in the inner parts of galaxies, while cosmological computer simulations indicate a steep power-law-like behaviour. This difference has become known as the “core/cusp problem,” and it remains one of the unsolved problems in small-scale cosmology.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f835ffe75dd37b87c57796d04c290e9a9f277946

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In Nuclear and High Energy Physics

Citations in the corpus

The distribution of dark matter in galaxies (2018, background): “…et al. 2005; Kuzio de Naray et al. 2008; de Blok et al. 2008; Oh et al. 2011; Adams et al. 2014 to name a few, reviews on this issue: Bullock and Boylan-Kolchin 2017; de Blok 2010).9 It is important to remark that the DM cores could come ab initio from the structural properties of the (exotic?)”
Modified Gravity and Cosmology (2011, methodology): “This is the cusp problem [366] and proposed solutions within the CDM paradigm include self-interacting dark matter [1174], fuzzy dark matter [628], or various feedback processes that expel dark matter.”
Cosmological Simulations with Self-Interacting Dark Matter I: Constant Density Cores and Substructure (2012, background): “…less concentrated and less cuspy than predicted in CDM simulations (e.g. Flores & Primack 1994; Simon et al. 2005; Kuzio de Naray et al. 2008; de Blok 2010; Dutton et al. 2011; Kuzio de Naray & Spekkens 2011; Oh et al. 2011; Walker & Peñarrubia 2011; Salucci et al. 2012; Castignani et al.…”
DARK AND LUMINOUS MATTER IN THINGS DWARF GALAXIES (2010, neutral): “A detailed observational review on where the “cusp/core” problem stands is given by Electronic address: seheon oh@ast.uct.ac.za Electronic address: edeblok@ast.uct.ac.za Electronic address: E.Brinks@herts.ac.uk Electronic address: walter@mpia.de Electronic address: robk@ast.cam.ac.uk 1 Department of”
Bar formation and evolution in disc galaxies with gas and a triaxial halo: morphology, bar strength and halo properties (2012, background): “…de Blok et al. 2001, 2008; de Blok & Bosma 2002; de Blok, Bosma & McGaugh 2003; Simon et al. 2003; Kuzio de Naray et al. 2006; Battaglia et al. 2008; Kuzio de Naray, McGaugh & de Blok 2008; Oh et al. 2008; de Blok 2010; Walker & Peñarrubia 2011; Amorisco & Evans 2012; Peñarrubia et al. 2012).”
“Non-cold” dark matter at small scales: a general approach (2017, background): “In fact, assuming the ΛCDM model, cosmological N -body simulations predict too many dwarf galaxies (missing satellite problem [2, 3]) and too much dark matter (DM) in the innermost regions of galaxies (cusp-core problem [4]) with respect to observations.”
Dark matter heats up in dwarf galaxies (2018, neutral): “By contrast, observations of gas-rich dwarf galaxy rotation curves have long favoured DM ‘cores’, with ρDM ∼ constant (Flores & Primack 1994; Moore 1994; de Blok 2010; Read et al. 2017).”
Dark matter halo merger histories beyond cold dark matter – I. Methods and application to warm dark matter (2012, background): “…and the inner slope of dark matter density profiles (Salucci 2001; Donato, Gentile & Salucci 2004; Donato et al. 2009; Newman et al. 2009, 2011; de Blok 2010; Kuzio de Naray & Kaufmann 2011; Kuzio de Naray & Spekkens 2011; Salucci et al. 2012; Wolf & Bullock 2012) and the apparent paucity of…”
Galaxy Masses: A Review (2013, background): “The inner shape parameter, α, is especially difficult to constrain observationally due to the added complication that only a small number of rotation curve points constrain this value; see (Dutton et al. 2005) and (de Blok 2010) for reviews.”
Dynamical modelling of the galactic bulge and bar: the Milky Way's pattern speed, stellar and dark matter mass distribution (2016, background): “How important those processes are is not yet settled, resulting in a cusp/core controversy similar to that in dwarf galaxies (Moore 1994; Burkert 1995; De Blok 2010).”
Dark matter and fundamental physics with the Cherenkov Telescope Array (2012, background): “In conclusion, observations of low surface brightness and dSphs [84, 85, 86] show that both cusped and cored profiles can accommodate their stellar dynamics.”