Maximum feedback and dark matter profiles of dwarf galaxies

By O. Gnedin, HongSheng Zhao. 2001

155 citations recorded by the source corpus.

The observed rotation curves of dark matter-dominated dwarf galaxies indicate low-density cores, contrary to the predictions of CDM models. A possible solution of this problem involves stellar feedback. A strong baryonic wind driven by vigorous star formation can remove a large fraction of the gas, causing the dark matter to expand. Using both numerical and analytical techniques, we explore the maximum effect of the feedback with an instantaneous removal of the gaseous disc. The energy input depends on the compactness of the disc, hence the specific angular momentum of the disc. For the plausible cosmological parameters and a wide range of the disc angular momenta, the feedback is insufficient to destroy the central halo cusp, while the inner density is lowered only by a modest factor of 2 to 6. Any realistic modelling of the feedback would have even lesser impact on dark matter. We find that no star formation effect can resolve the problems of CDM cusps.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/d8618abf8107c8282b4cb0cc906f1a8aa91a5001

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In Statistical and Nonlinear Physics

Citations in the corpus

The spatial distribution of the Milky Way and Andromeda satellite galaxies (2006, background): “Even extreme baryon removal cannot evolve a cusped to a cored DM halo (Gnedin & Zhao 2002).”
Galaxies as simple dynamical systems: observational data disfavor dark matter and stochastic star formation (2014, background): “[210] studied this problem using simulations and analytical approaches and conclude “We find that no star formation effect can resolve the problems of CDM cusps.”
Small scale problems of the $\Lambda$CDM model: a short review (2016, background): “[290] showed that, while a single explosive event did not move sufficient energy to form a core, repeated moderately violent explosions could reach the goal (however see [291] for a different point of view).”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, background): “…the following conditions: (1) By removing large amounts of baryons on a timescale much faster than in which they were accumulated (e.g., Navarro et al. 1996b; Gnedin & Zhao 2002; Read & Gilmore 2005; Governato et al. 2010); or (2) By inducing large scale bulk motions (Mashchenko et al. 2006; 2008).”
Cuspy No More: How Outflows Affect the Central Dark Matter and Baryon Distribution in Lambda CDM Galaxies (2012, background): “In fact, some studies were not able to create cores using single, massive blowouts (Gnedin & Zhao 2002; Boylan-Kolchin et al. 2011a).”
A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, background): “…in recent years that baryonic processes can alter the distributions of dark matter within halos, potentially steepening (Blumenthal et al. 1986; Gnedin & Zhao 2002; Gnedin et al. 2011) or flattening (Navarro et al. 1996; Read & Gilmore 2005; Mashchenko et al. 2006, 2008; Governato et al. 2010;…”
Mass loss from dwarf spheroidal galaxies: the origins of shallow dark matter cores and exponential surface brightness profiles (2004, methodology): “Navarro et al. (1996a), Gelato & Sommer-Larsen (1999) and Gnedin & Zhao (2002) have all looked at the effect on a Hernquist halo density profile of removing a baryon disc.”
How supernova feedback turns dark matter cusps into cores (2011, background): “The picture is related to the more established view that removal of baryons through galactic superwinds could cause the central dark matter profile to flatten (e.g. Navarro et al. 1996a; Gnedin & Zhao 2002; Read & Gilmore 2005).”
AGN-driven quenching of star formation: morphological and dynamical implications for early-type galaxies (2013, background): “…2006; Peirani, Kay & Silk 2008; Pontzen & Governato 2012; Teyssier et al. 2013), in conjunction with the adiabatic expansion of DM and stars (Blumenthal et al. 1986; Gnedin & Zhao 2002; Gnedin et al. 2004) produced by the decrease of the gas density due to AGN feedback in the centre of DM haloes.”
Dynamical Evolution of Galaxies in Clusters (2003, background): “(15) It describes very well the rate of heating in simulations, even including the resonant interactions of stars (see the discussion in Gnedin & Zhao 2002, based on the results of Weinberg 1993).”
The unexpected diversity of dwarf galaxy rotation curves (2015, background): “An alternative is that rotation curves may be reconciled with CDM haloes by ‘baryon effects’ operating during the formation of a galaxy (Navarro, Eke & Frenk 1996; Gnedin & Zhao 2002; Read & Gilmore 2005).”
The formation of disc galaxies in high-resolution moving-mesh cosmological simulations (2013, background): “Gnedin & Zhao (2002) however showed that even for assumptions of maximum feedback the central halo cusp could not be destroyed by outflows, with the inner density lowered only by a moderate factor.”
A wide-field H I mosaic of Messier 31 - II. The disk warp, rotation, and the dark matter halo (2009, background): “This has given new insights on the nature of dark matter and lead to discussion on how the halo structure might have been altered by the galaxy formation process (e.g. Gnedin & Zhao 2002).”
THE CENTRAL SLOPE OF DARK MATTER CORES IN DWARF GALAXIES: SIMULATIONS VERSUS THINGS (2010, background): “A rapid change in potential (faster than the dynamical time) due to star burst triggered outflows, is one mechanism which has been shown to be capable of transforming cusp–like profiles into (flatter) cores (Navarro et al. 1996; Read & Gilmore 2005 although see Gnedin & Zhao 2002).”
Understanding the shape and diversity of dwarf galaxy rotation curves in ΛCDM (2016, background): “They found that, for reasonable initial conditions and gas collapse factors, the effect of a single burst is very small (see also Gnedin & Zhao 2002).”
The Milky Way’s bright satellites as an apparent failure of ΛCDM (2011, result): “Gnedin & Zhao (2002) demonstrated that removal of a gaseous disk containing nearly all of a dwarf galaxy’s baryons will reduce the central dark matter density by approximately 50%; our reduction of ∼ 25% in Vcirc is in good agreement with this result.”
The Orbital Poles of Milky Way Satellite Galaxies: A Rotationally Supported Disk of Satellites (2008, background): “No physical mechanism has been found that can evolve cusps to cores (Gnedin & Zhao 2002).”