Halo Response to Galaxy Formation
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Baryons can cause a DM halo to contract, as known for a long time and confirmed by many subsequent studies.
“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 Barnes 1987
Cites
Core condensation in heavy halos: a two-stage theory for galaxy formation and clustering
White, S. D. M., & Rees, M. J. (1978) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/183.3.341 · Cited by 3,919 · see citing works
The structure of star clusters. III. Some simple dvriamical models
King, I. R. (1966) · The Astronomical Journal · doi:10.1086/109857 · Cited by 1,926 · see citing works
Contraction of dark matter galactic halos due to baryonic infall
Blumenthal, G. R., Faber, S. M., Flores, R., & Primack, J. R. (1986) · The Astrophysical Journal · doi:10.1086/163867 · Cited by 1,213 · see citing works
Formation and rotation of disc galaxies with haloes
Fall, S. M., & Efstathiou, G. (1980) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/193.2.189 · Cited by 944 · see citing works
Bosma, A. (1981) · The Astronomical Journal · doi:10.1086/113062 · Cited by 365 · see citing works
The distribution of mass in spiral galaxies
Burstein, D., & Rubin, V. C. (1985) · The Astrophysical Journal · doi:10.1086/163541 · Cited by 108 · see citing works
Some possible regularities in the missing mass problem
Bahcall, J. N., & Casertano, S. (1985) · The Astrophysical Journal · doi:10.1086/184480 · Cited by 103 · see citing works
The response of a spheroid to a disc field or were bulges ever ellipticals?
Barnes, J., & White, S. D. M. (1984) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/211.4.753 · Cited by 98 · see citing works
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The milky way total mass profile as inferred from Gaia DR2
Cautun, M., Benítez-Llambay, A., Deason, A. J., Frenk, C. S., Fattahi, A., Gómez, F. A., Grand, R. J. J., Oman, K. A., Navarro, J. F., & Simpson, C. M. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa1017 · Cited by 332 · see citing works
“…is well described by the adiabatic contraction model (Callingham et al. 2019a), 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 (Barnes & White 1984; Blumenthal et al. 1986; Barnes 1987).”
BackgroundThe Milky Way total mass profile as inferred from Gaia DR2
Cautun, M., Benitez-Llambay, A., Deason, A. J., Frenk, C. S., Fattahi, A., Gómez, F. A., Grand, R. J. J., Oman, K. A., Navarro, J. F., & Simpson, C. M. (2019) · arXiv · doi:10.48550/arxiv.1911.04557 · Cited by 335
Galaxy-induced transformation of dark matter haloes: Transformations of CDM haloes
Abadi, M. G., Navarro, J. F., Fardal, M., Babul, A., & Steinmetz, M. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16912.x · Cited by 237 · see citing works
Maximal Disks and the Tully‐Fisher Relation
Courteau, S., & Rix, H. (1999) · The Astrophysical Journal · doi:10.1086/306872 · Cited by 218 · see citing works
The Disk and Dark Halo Mass of the Barred Galaxy NGC 4123. II. Fluid‐Dynamical Models
Weiner, B. J., Sellwood, J. A., & Williams, T. B. (2001) · The Astrophysical Journal · doi:10.1086/318289 · Cited by 169 · see citing works
Mass discrepancies in galaxies: dark matter and alternatives
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The Compression of Dark Matter Halos by Baryonic Infall
Sellwood, J. A., & McGaugh, S. S. (2005) · The Astrophysical Journal · doi:10.1086/491731 · Cited by 164 · see citing works
THE CUSP/CORE PROBLEM AND THE SECONDARY INFALL MODEL
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DARK MATTER DENSITIES DURING THE FORMATION OF THE FIRST STARS AND IN DARK STARS
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A revised Λ CDM mass model for the Andromeda Galaxy
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Barnes, J. E. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv2381 · Cited by 23 · see citing works
Self-citationIncorporating baryon-driven contraction of dark matter halos in rotation curve fits
Li, P., McGaugh, S., Lelli, F., Schombert, J. M., & Pawlowski, M. S. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243916 · Cited by 19 · see citing works
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Systematic Properties of Rotation Curves and Dark Matter
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Realization of Swift and Expressive Chat in CSCL: Reach Project
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Galaxy Rotation Curves in the Context of LambdaCDM Cosmology
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Dissipation and Formation of Galactic Halos
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- Authors
- Barnes, J. E.
- Corresponding author
- Barnes, Joshua E.
- ORCID
- Barnes, Joshua E.
- Venue
- Nearly Normal Galaxies
- Publisher
- Springer New York
- Published
- 1987
- Pages
- 154-159
- OpenAlex
- W1521072419
- Cited by
- 22
- References
- 8
- Citations by year
- 2022: 1 · 2020: 1 · 2015: 1 · 2014: 1
- FWCI
- 9.33
- Type
- book chapter
- Language
- en
- Open access
- closed
- Locations
- Springer eBooks (publishedVersion)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Keywords
- galaxy halos, flat rotation curves, disk formation, dark halo, fine-tuning problem, halo orbits, galaxy formation
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
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