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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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“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)
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BackgroundDARK MATTER ANNIHILATION AND PRIMORDIAL STAR FORMATION
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“…based on the initial angular momentum of the gas and the halo profile, assuming that angular momentum is conserved and that the self-gravity of the collapsing baryons causes contraction of the matter in the inner part of the halo (Blumenthal et al. 1986; Flores et al. 1993; Mo, Mao & White 1998).”
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“The halo term vh is computed by assuming that the halo follows an NFW profile modified by adiabatic contraction (Blumenthal et al. 1986).”
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“The code implements also the recipe of Blumenthal et al. (1986) to mimic the adiabatic contraction of the smooth dark matter halo, due to the growth of the central galaxy.”
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“…model this is to assume an adiabatic contraction of the halo, which remains spherical, so that the angular momentum of individual particles is conserved (see Barnes & White 1984, Blumenthal et al. 1986 and Navarro & Steinmetz 2000 for more details and numerical tests on the validity of this model).”
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“Blumenthal et al. (1986) described an approximate analytical model to calculate the effects of AC.”
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“…to affect the density distribution of dark matter, but the effects are far from being clear: the best studied process is adiabatic contraction (Blumenthal et al. 1986, Gnedin et al 2004, Sellwood & McGaugh 2005), which would make the halos more centrally concentrated, but mechanisms with…”
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“Adding a dissipative baryon component makes mass distributions even more concentrated (Blumenthal et al. 1986; Dubinski 1994).”
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“When baryons cool slowly and accumulate at the centre of a DM halo, they steepen the potential well, leading to an adiabatic contraction of the DM distribution and even more severe cusps (Blumenthal et al. 1986; Gnedin et al. 2004; Oñorbe et al. 2007).”
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“Adiabatic Contraction (AC) (Blumenthal et al. 1986; Ryden & Gunn 1987; Gnedin et al. 2004) may cause a steepening of the inner slope of the dark matter density profile as the gas condenses and sinks to to the center of the dark matter potential well (Diemand et al. 2004; Fukushige et al. 2004; Reed…”
BackgroundEffective theory of self-interacting dark matter
Bellazzini, B., Cliche, M., & Tañedo, P. (2013) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.88.083506 · Cited by 60
Vikhlinin, A. A., Kravtsov, A. V., Markevich, M., Sunyaev, R., & Churazov, E. (2014) · Physics-Uspekhi · doi:10.3367/ufne.0184.201404a.0339 · Cited by 61
Primack, J. R. (2009) · New Journal of Physics · doi:10.1088/1367-2630/11/10/105029 · Cited by 63
Self-citationDARK STARS: A NEW LOOK AT THE FIRST STARS IN THE UNIVERSE
Spolyar, D., Bodenheimer, P., Freese, K., et al. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/705/1/1031 · Cited by 60
“Paper I used a simple Blumenthal method, which assumes circular particle orbits (Blumenthal et al. 1986; Barnes & White 1984; Ryden & Gunn 1987) to obtain estimates of the density.”
MethodTime-delay cosmographic forecasts with strong lensing and JWST stellar kinematics
Yıldırım, A., Suyu, S. H., & Halkola, A. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa498 · Cited by 71
Galactic Center Excess in γ Rays from Annihilation of Self-Interacting Dark Matter
Kaplinghat, M., Linden, T., & Yu, H.-B. (2015) · Physical Review Letters · doi:10.1103/physrevlett.114.211303 · Cited by 59
Knebe, A., Libeskind, N. I., Knollmann, S. R., et al. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16514.x · Cited by 59
“After all, the inclusion of baryons should affect the dark matter, too: Blumenthal et al. (1986) showed that dissipative baryons will lead directly to the adiabatic contraction of haloes (see also Gnedin et al. 2004) and should th s be a critical ingredient in determining halo and subhalo prope…”
BackgroundCores and revived cusps of dark matter haloes in disc galaxy formation through clump clusters
Inoue, S., & Saitoh, T. R. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19873.x · Cited by 59
“Contrary to the result of Spano et al. (2008), on the other hand, some theoretical studies have proposed that central density profile of DM halo of massive galaxies become steeper rather than shallower by adiabatic contraction of baryonic gas (e.g. Blumenthal et al. 1986; Gnedin & Zhao 2002).”
ResultThe baryons in the Milky Way satellites
Parry, O. H., Eke, V. R., Frenk, C. S., & Okamoto, T. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2011.19971.x · Cited by 59
“Central concentrations of cold baryonic matter can induce an adiabatic, radial contraction of the central regions (Blumenthal et al. 1986; Gnedin et al. 2004), while the opposite effect can be achieved if dense clumps of baryonic material heat the central distribution of dark matter (Mo & Mao 2004;…”
BackgroundNIHAO XII: galactic uniformity in a ΛCDM universe
Dutton, A. A., Obreja, A., Wang, L., Gutcke, T. A., Buck, T., Udrescu, S. M., Frings, J., Stinson, G. S., Kang, X., & Macciò, A. V. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx458 · Cited by 59
“However, Dutton et al. (2007, 2011) showed that when models are constrained to reproduce the sizes of galaxies, they also overpredict the circular velocities if haloes contract in response to galaxy formation (Blumenthal et al. 1986; Gnedin et al. 2004).”
BackgroundAlabi, A., Forbes, D. A., Romanowsky, A. J., Brodie, J. P., Strader, J., Janz, J., Usher, C., Spitler, L. R., Bellstedt, S., & Ferré-Mateu, A. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx678 · Cited by 59
“G through adiabatic halo contraction (e.g. Blumenthal et al. 1986) or halo expansion through gravitational heating from infalling gas clumps (e.g. Johansson et al. 2009) or outflows linked to feedback events (e.g Macciò et al. 2012).”
Backgroundmoka: a new tool for strong lensing studies
Giocoli, C., Meneghetti, M., Bartelmann, M., Moscardini, L., & Boldrin, M. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20558.x · Cited by 61
“Blumenthal et al. (1986) have described the adiabatic contraction analytically, finding good agreement with numerical simulations.”
ResultDark Matter Halos of Disk Galaxies: Constraints from the Tully-Fisher Relation
Gnedin, O. Y., Weinberg, D. H., Pizagno, J., Prada, F., & Rix, H. (2006) · CERN Document Server (European Organization for Nuclear Research) · Cited by 57
Ionized Gas in Damped Lyα Protogalaxies. II. Comparison between Models and the Kinematic Data
Wolfe, A. M., & Prochaska, J. X. (2000) · The Astrophysical Journal · doi:10.1086/317859 · Cited by 59
Decomposition of the visible and dark matter in the Einstein ring 0047-2808 by semi-linear inversionPreprint
Dye, S., & Warren, S. J. (2004) · Cited by 59
LUMINOUS SATELLITES OF EARLY-TYPE GALAXIES. I. SPATIAL DISTRIBUTION
Nierenberg, A. M., Auger, M. W., Treu, T., et al. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/731/1/44 · Cited by 58
“However, the inner region of the host halo profile is likely to be steeper in the presence of baryons (e.g., Blumenthal et al. 1986; Gnedin et al. 2004).”
BackgroundSterile neutrino portal to Dark Matter I: the U(1) B-L case
Escudero, M., Rius, N., & Veronica Sanz, B. (2017) · Sussex Research Online (University of Sussex) · Cited by 56
Dark matter direct search rates in simulations of the Milky Way and Sagittarius stream
Purcell, C. W., Zentner, A. R., & Wang, M.-Y. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/08/027 · Cited by 56
“A simple proposal would be to employ a model for adiabatic halo contraction [68, 69] on the original host halo, which is well described by the standard NFW profile form.”
MethodORBIT-BASED DYNAMICAL MODELS OF THE SOMBRERO GALAXY (NGC 4594)
Jardel, J. R., Gebhardt, K., Shen, J., Fisher, D. B., Kormendy, J., Kinzler, J., Lauer, T. R., Richstone, D., & Gültekin, K. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/739/1/21 · Cited by 58
“We interpret this as the result of severe compression of the halo by the gravity of the baryons (Blumenthal et al. 1986).”
BackgroundOn the universality of density profiles
Popolo, A. D. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17288.x · Cited by 58
“…with universality of dark matter profiles do not study the possible effects produced by the presence of baryons, whose effect is to shallow (El-Zant et al. 2001, 2004; Romano-Diaz et al. 2008) and to steepen (Blumenthal et al. 1986; Gnedin et al. 2004; Klypin et al. 2002) the dark matter profile.”
BackgroundMerger-induced galaxy transformations in the artemis simulations
Dillamore, A. M., Belokurov, V. A., Font, A. S., & McCarthy, I. G. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac1038 · Cited by 57
Astrophysical tests of dark matter self-interactions
Adhikari, S., Banerjee, A., Boddy, K. K., Cyr-Racine, F.-Y., Desmond, H., Dvorkin, C., Jain, B., Kahlhoefer, F., Kaplinghat, M., Nierenberg, A., et al. (2025) · Reviews of Modern Physics · doi:10.1103/m2vm-59y3 · Cited by 156
Napolitano, N. R., Pota, V., Romanowsky, A. J., Forbes, D. A., Brodie, J. P., & Foster, C. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stt2484 · Cited by 57
“We do not explore stronger AC recipes (e.g. Blumenthal et al. 1986), which might allow lower stellar mass normalization by dragging more DM into the central regions (see e.g. Napolitano, Romanowsky & Tortora 2010), as these seem to be disfavoured by both simulations (e.g. Abadi et al. 2010) and…”
BackgroundSize matters: abundance matching, galaxy sizes, and the Tully–Fisher relation in EAGLE
Ferrero, I., Navarro, J. F., Abadi, M. G., Sales, L. V., Bower, R. G., Crain, R. A., Frenk, C. S., Schaller, M., Schaye, J., & Theuns, T. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw2691 · Cited by 57
“…https://academic.oup.com/mnras/article-abstract/464/4/4736/2417418 by Jacob Heeren user on 11 January 2018 Modelling the halo response as ‘adiabatic contraction’ (Barnes & White 1984; Blumenthal et al. 1986) yields the individual symbols and the thick solid curve in the right-hand panel of Fig.”
BackgroundSubhalo demographics in the Illustris simulation: effects of baryons and halo-to-halo variation
Chua, K. T. E., Pillepich, A., Rodríguez-Gómez, V., Vogelsberger, M., Bird, S., & Hernquist, L. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx2238 · Cited by 57
“In early analytical work on the baryonic back-reaction on DM haloes, Blumenthal et al. (1986) found that the condensation of baryons at halo centers can result in DM haloes that are more centrally concentrated, in a process known such as adiabatic contraction.”
BackgroundComplementarity of direct dark matter detection and indirect detection through gamma rays
Bergström, L., Bringmann, T., & Edsjö, J. (2011) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.83.045024 · Cited by 56
The empirical case for 10-GeV dark matter
Hooper, D. (2012) · Physics of the Dark Universe · doi:10.1016/j.dark.2012.07.001 · Cited by 67
Search for dark matter towards the Galactic Centre with 11 years of ANTARES data
Albert, A., Andre, M. L., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J. J., Aublin, J., Baret, B., Basa, S., Belhorma, B., et al. (2020) · Physics Letters B · doi:10.1016/j.physletb.2020.135439 · Cited by 68
“[4, 5, 6, 7]).”
Formation of elongated galaxies with low masses at high redshift
Ceverino, D., Primack, J. R., & Dekel, A. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1603 · Cited by 56
Self-citationSystematic variations of central mass density slopes in early-type galaxies
Tortora, C., Barbera, F. L., Napolitano, N. R., et al. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu1616 · Cited by 56
“Gas and stars, falling down into the DM potential well, could drag a significant amount of DM particles inside, making the DM profile more concentrated in the galaxy centre (Blumenthal et al. 1986; Gnedin et al. 2004; Del Popolo 2009; Cardone et al. 2011b) than the “expected” NFW law.”
Background
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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