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Contraction of dark matter galactic halos due to baryonic infall
Abstract
Varied evidence suggests that galaxies consist of roughly 10 percent baryonic matter by mass and that baryons sink dissipatively by about a factor of 10 in. radius during galaxy formation. It is shown that such infall strongly perturbs the underlying dark matter distribution, pulling it inward and creating cores that are considerably smaller and denser than would have evolved without dissipation. Any discontinuity between the baryonic and dark matter mass distributions is smoothed out by the coupled motions of the two components. If dark halos have large core radii in the absence of dissipation, the above infall scenario yields rotation curves that are flat over large distances, in agreement with observations of spiral galaxies. Such large dissipationless cores may plausibly result from large internal kinetic energy in protogalaxies at maximum expansion, perhaps as a result of subclustering, tidal effects, or anisotropic collapse.
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In the citing paper
“For MW and higher mass haloes, the effect of baryons on the DM halo is well described by the adiabatic contraction model (Callingham et al. 2020), in which baryons slowly accumulate at the halo centre and the DM distribution distorts in such a way that its action integrals remain approximately constant”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Blumenthal et al. 1986
In the citing paper
“Other simpler adiabatic contraction approximations, such as those used by Blumenthal et al. (1986) and Gnedin et al. (2004), tend systematically to under- or overpredict the halo contraction (e.g. Abadi et al. 2010; Duffy et al. 2010; Pedrosa et al. 2010; Dutton et al. 2016; Artale et al. 2019).”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Blumenthal et al. 1986
In the citing paper
“That baryons can cause a DM halo to contract has been known for a long time (Blumenthal et al. 1986; Barnes 1987), and this has been confirmed by many subsequent studies”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Blumenthal et al. 1986
In the citing paper
“and that roughly agrees with the Blumenthal et al. (1986) and Gnedin et al. (2004) adiabatic contraction approximations, although we do find systematic deviations at the 10% level.”
From The milky way total mass profile as inferred from Gaia DR2 (2020) · cites this paper as Blumenthal et al. (1986)
Citations
Cited by
Sorted by citations
The Structure of Cold Dark Matter Halos
Navarro, J. F., Frenk, C. S., & White, S. D. M. (1996) · The Astrophysical Journal · doi:10.1086/177173 · Cited by 8,544
Jungman, G., Kamionkowski, M., & Griest, K. (1996) · Physics Reports · doi:10.1016/0370-1573(95)00058-5 · Cited by 4,171
Profiles of dark haloes: evolution, scatter and environment
Bullock, J. S., Kolatt, T., Sigad, Y., Somerville, R. S., Kravtsov, A. V., Klypin, A. A., Primack, J. R., & Dekel, A. (2001) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2001.04068.x · Cited by 2,328
“…qualitative understanding of how profile characteristics may affect galactic disc formation, we may assume that an exponential disc forms by the adiabatic contraction of gas inside the dark-matter halo (Blumenthal et al. 1986; Flores et al. 1993; Dalcanton, Spergel, & Summers 1997; Mo et al. 1998).”
BackgroundSelf-citationHow do galaxies get their gas?
Kere, D., Katz, N. S., Weinberg, D. H., & Davé, R. (2005) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2005.09451.x · Cited by 2,267
Cole, S., Lacey, C. G., Baugh, C. M., & Frenk, C. S. (2002) · Monthly Notices of the Royal Astronomical Society · doi:10.1046/j.1365-8711.2000.03879.x · Cited by 1,952
“This adiabatic invariance method for calculating the response of a halo or spheroid to the disk was originally developed and applied by Barnes & White (1984), Blumenthal et al. (1986) and Ryden & Gunn (1987).”
Method
Metadata
- Authors
- Blumenthal, G. R., Faber, S. M., Flores, R., & Primack, J. R.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 1986-02
- Volume
- 301
- Pages
- 27
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2083950714
- Cited by
- 1,213
- References
- 0
- Citations by year
- 2026: 17 · 2025: 32 · 2024: 28 · 2023: 27 · 2022: 36 · 2021: 47 · 2020: 49 · 2019: 39 · 2018: 43 · 2017: 39 · 2016: 55 · 2015: 51 · 2014: 52 · 2013: 58 · 2012: 83
- FWCI
- 18.18
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- The Astrophysical Journal (publishedVersion)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Dark Matter and Cosmic Phenomena
- Keywords
- dark matter halos, energy dissipation, halo cores, rotation curves, spiral galaxies, galaxy formation, protogalaxies, subclustering, tidal effects, anisotropic collapse
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