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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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Stellar feedback and the energy budget of late-type Galaxies: missing baryons and core creation
Katz, H., Desmond, H., Lelli, F., McGaugh, S., Cintio, A. D., Brook, C. B., & Schombert, J. M. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty2129 · Cited by 12
“…the most well-studied effects of feedback is how the density profile of the dark matter halo responds to large-scale inflows or outflows of baryons (Blumenthal et al. 1986; Navarro, Frenk & White 1996b; Gnedin et al. 2004; Read & Gilmore 2005; Pontzen & Governato 2012; Martizzi, Teyssier & Moore…”
BackgroundConstraints on MOND from the lensing cluster MS2137-23
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“See also e.g. Blumenthal et al (1986); Keeton (2001)) Nevertheless, figure 2 reveals discrepancies outside the cluster area probe by the radial and the tangential arc.”
BackgroundChae, K. (2002) · The Astrophysical Journal · doi:10.1086/339164 · Cited by 13
“Moreover, mass distributions in the inner regions of the galaxies are expected to be modified because of the effects of the baryons (e.g., Blumenthal et al. 1986; Mo, Mao, &White 1998; Cole et al. 2000; Gonzalez et al. 2000; Kochanek & White 2001).”
BackgroundA Model for the Density Distribution of Virialized Cold Dark Matter Halos
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“This assumption is based on the fact that for periodic orbits ∮ pdq (where p and q are then conjugate momentum and coordinate, respectively) is an adiabatic invariant (Blumenthal et al. 1986, Flores et al. 1993).”
BackgroundTwo phase galaxy formation: The Gas Content of Normal GalaxiesPreprint
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“Nevertheless, more recent and realistic simulations that include also the physics of baryons (e.g. Blumenthal et al. 1986; El-Zant, Shlosman & Hoffman 2001; Jesseit, Naab & Burkert 2002; Bertin, Liseikina & Pegoraro 2003; Gnedin et al. 2004; Ma & Boylan-Kolchin 2004; Duffy et al. 2010), like…”
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“For the Blumenthal et al. (1986) case (top), there is clearly a disagreement between observationally inferred and contracted profiles.”
BackgroundInfluentialGeometrical aspects on the dark matter problem
Capistrano, A. J. S., & Cabral, L. A. (2014) · Annals of Physics · doi:10.1016/j.aop.2014.05.013 · Cited by 13
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“Comparisons with the earlier work of Blumenthal et al.(1986) showed that the assumption of spherical symmetry induces a systematic over-prediction of the density enhancement in the inner 5% of the virial radius.”
BackgroundMethodResultA Universal Angular Momentum Profile for Dark Matter Halos
Liao, S., Jianxiong, C., & Chu, M. C. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa79fb · Cited by 12
“Analytical (e.g. Blumenthal et al. 1986) as well as numerical studies (e.g. Dutton et al. 2016) show that galaxy formation processes can alter the inner dark matter density profile predicted by dark-matter-only N-body simulations.”
BackgroundDark matter haloes in the multicomponent model – II. Density profiles of galactic haloes
Todoroki, K., & Medvedev, M. V. (2018) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sty3353 · Cited by 12
The Parallelism between Galaxy Clusters and Early-type Galaxies. I. The Light and Mass Profiles
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“[45] G.”
BackgroundThe Dark Halo of NGC 5963 as a Constraint on Dark Matter Self‐Interaction at the Low‐Velocity Regime
Sánchez-Salcedo, F. J. (2005) · The Astrophysical Journal · doi:10.1086/432593 · Cited by 12
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BackgroundMethodBerry, M., Somerville, R. S., Gawiser, E., et al. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw231 · Cited by 12
“…of the disc is computed based on the initial angular momentum of the gas and the halo profile, assuming angular momentum is conserved and the self-gravity of the collapsing baryons causes contraction in the inner part of the halo (Blumenthal et al. 1986; Flores et al. 1993; Mo, Mao & White 1998).”
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Bringmann, T. (2005) · KTH Publication Database DiVA (KTH Royal Institute of Technology) · Cited by 12
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BackgroundConnecting the Local Stellar Halo and Its Dark Matter Density to Dwarf Galaxies via Blue Stragglers
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“+MDM MDM Rh,s (9) (e.g., Blumenthal et al. 1986; Forbes et al. 2018), which has virtually no effect since for this sample of dwarf galaxies M? is order of magnitudes smaller than MDM.”
BackgroundMultiscatter capture of superheavy dark matter by Pop III stars
Ilie, C., & Zhang, S. (2019) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2019/12/051 · Cited by 11
“Adiabatic contraction [11] is a mechanism that is responsible for driving up the density of dark matter at the center of a collapsing gas cloud.”
BackgroundBaryon-driven decontraction in Milky Way-mass haloes
Moreno, V. J. F., Benítez-Llambay, A., Cole, S., & Frenk, C. S. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac312 · Cited by 13
Tracking the orbit of unresolved subhaloes for semi-analytic models
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“Blumenthal et al. (1986) argued that such a conspiracy will arise naturally if the dissipational collapse of baryons is limited by their initial angular momentum and if the baryon fraction is roughly equal to the spin parameter λ = JE1/2G−1M−5/2.”
BackgroundSelf-citationGamma-ray constraints on the first stars from annihilation of light WIMPs
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“In addition, the response of dark matter to baryon cooling must be included and is often modelled with adiabatic contraction (Blumenthal et al. 1986).”
The Distribution of Dark Mass in Galaxies
Sackett, P. D. (1996) · Springer eBooks · doi:10.1007/978-94-009-0221-3_45 · Cited by 11
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“The latter assumes that the baryons contracted adiabatically and symmetrically within the pre-existing dark matter halo, compressing the dark matter and increasing its density [56].”
Cousin, M., Buat, V., Boissier, S., Béthermin, M., Roehlly, Y., & Génois, M. (2016) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201527734/pdf · Cited by 15
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BackgroundCan we use weak lensing to measure total mass profiles of galaxies on 20 kpc scales?
Kobayashi, M. I. N., Leauthaud, A., More, S., Okabe, N., Laigle, C., Rhodes, J. D., & Takeuchi, T. T. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv424 · Cited by 10
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BackgroundDark stars and boosted dark matter annihilation rates
Ilie, C., Freese, K., & Spolyar, D. (2011) · New Journal of Physics · doi:10.1088/1367-2630/13/5/053050 · Cited by 10
“We use the Blumenthal method (Barnes & White 1984; Blumenthal et al. 1986; Ryden & Gunn 1987) to calculate the adiabatic compression of the halo.”
MethodModeling the dynamical friction timescale of a sinking satellite
Gan, J.-L., Kang, X., Hou, J., & Chang, R. (2010) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/10/12/005 · Cited by 10
“Some found that central density increases (e.g., Blumenthal et al., 1986; Gnedin et al., 2004), but some disagreed with it.”
BackgroundHigh-redshift microlensing and the spatial distribution of dark matter in the form of MACHOs
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“The general expectation is that baryon cooling inside CDM halos will cause the dark halos to contract (Blumenthal et al. 1986; Gnedin et al. 2004; Sellwood & McGaugh 2005), although bar formation could possibly drive the evolution of the innermost part of dark halo in the opposite direction (e.g.…”
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Ando, S., Kavanagh, B. J., Macías, O., et al. (2019) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2019/10/040 · Cited by 10
“Adiabatic contraction acts to increase the density in the center of the host galaxy [39, 40] while tidal disruption acts to remove mass from the subhalos, a process which is more efficient in the dense central region of the host halo.”
BackgroundBoyce, E. R., Winn, J. N., Hewitt, J. N., & Myers, S. T. (2006) · The Astrophysical Journal · doi:10.1086/505640 · Cited by 10
“Adiabatic contraction (Blumenthal et al. 1986) and similar models (Sellwood & McGaugh 2005) model the contraction of dark matter under the gravitation of a baryonic disk or bulge.”
MethodEffects of galaxy-halo alignment and adiabatic contraction on gravitational lens statisticsPreprint
Minor, Q. E., & Kaplinghat, M. (2008) · Cited by 10
Matter power spectra in dynamical dark energy cosmologiesPreprint
Fedeli, C., Dolag, K., & Moscardini, L. (2012) · Cited by 10
Kumar, J., Maurya, S. K., Kiroriwal, S., Errehymy, A., Myrzakulov, K., & Umbetova, Z. (2024) · Physics of the Dark Universe · doi:10.1016/j.dark.2024.101636 · Cited by 9
de Denus-Baillargeon, M.-M., Hernandez, O., Boissier, S., et al. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/773/2/173 · Cited by 9
“The dissipation of the disc, via infall of baryons, is thought to compress the dark halo distribution through adiabatic contraction (Blumenthal et al. 1986).”
BackgroundThe relationship between galaxy and halo sizes in the Illustris and IllustrisTNG simulations
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Dark Matter halo parameters from overheated exoplanets via Bayesian hierarchical inference
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Provenza, A., Quirós, M., & Ullio, P. (2006) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2006/12/007 · Cited by 9
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“(We note that we have not included adiabatic contraction (e.g., Blumenthal et al. 1986; Gnedin et al. 2004) of the DM halo in our model which would lead to an even larger concentration.)”
BackgroundA multi-frequency analysis of possible dark matter contributions to M31 gamma-ray emissions
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Halos and Angular Momentum Generation
Frenk, C. S. (1987) · Springer eBooks · doi:10.1007/978-1-4612-4762-3_47 · Cited by 9
String-Seeded Spirals: Origin of Rotation and the Density of the Halo
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NIHAO – XXVIII. Collateral effects of AGN on dark matter concentration and stellar kinematics
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“Although the baryons are not dynamically significant for the galaxies we consider and the adiabatic contraction effect (Blumenthal et al., 1986; Gnedin et al., 2004) is negligible for the CDM halo, they do have a mild impact on the SIDM halo, as we will show in Sec.”
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“…can also be observed in dark matter substructures which become less sensitive to tidal torques and will survive a longer time in their host haloes, as has been extensively discussed in the past literature (Blumenthal et al. 1986; Gnedin et al. 2004; Duffy et al. 2010 and references therein).”
BackgroundLi, S., Li, R., Zhu, K., Lu, S., Cappellari, M., Mao, S., Wang, C., & Gao, L. (2024) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stae838 · Cited by 8
THE DARK MATTER HALO CONCENTRATION AND STELLAR INITIAL MASS FUNCTION OF A CASSOWARY GROUP
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BackgroundDark halo microphysics and massive black hole scaling relations in galaxies
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“It may be necessary for baryons to become denser than some threshold, in order to pinch the DM (via adiabatic contraction, Blumenthal et al. 1986) and enable collapse of the innermost DM.”
BackgroundDiagnostics of baryonic cooling in lensing galaxies
Leier, D., Ferreras, I., & Saha, P. (2012) · Zurich Open Repository and Archive (University of Zurich) · doi:10.5167/uzh-70271 · Cited by 8
Hughes, M. E., Jethwa, P., Hilker, M., van de Ven, G., Martig, M., Pfeffer, J., Bastian, N., Kruijssen, J. M. D., Trujillo-Gomez, S., Reina-Campos, M., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab196 · Cited by 8
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Velmani, P., & Paranjape, A. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad297 · Cited by 12
Angular momentum evolution in dark-matter haloes
Book, L. G., Brooks, A. M., Peter, A. H. G., Benson, A. J., & Governato, F. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.17824.x · Cited by 8
“Occasionally, the assumption of circular orbits is swapped in favor of choosing a variant of the radial action as a conserved quantity (Blumenthal et al. 1986; Gnedin et al. 2004).”
BackgroundSatellite Survival in Cold Dark Matter Cosmology
Boily, C. M., Nakasato, N., Spurzem, R., et al. (2004) · The Astrophysical Journal · doi:10.1086/423421 · Cited by 8
“Several studies have argued for a more spherical morphology in the inner region of haloes (e.g., Blumenthal et al. 1986; Dubinsky 1994).”
BackgroundTHE RINGS SURVEY. I. HαAND H i VELOCITY MAPS OF GALAXY NGC 2280
Mitchell, C. J., Williams, T. B., Spekkens, K., Lee-Waddell, K., de Naray, R. K., & Sellwood, J. A. (2015) · The Astronomical Journal · doi:10.1088/0004-6256/149/3/116 · Cited by 9
“The extra central attraction of the baryons in the inner parts causes the DM halo to contract adiabatically, increasing its inner density (Blumenthal et al. 1986; Gnedin et al. 2004; Sellwood & McGaugh 2005).”
BackgroundSmith, R. J., Lucey, J. R., & Edge, A. C. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx059 · Cited by 8
“The slope of the DM profile towards the cluster centre is sensitive to the micro-physics of the DM particle (Spergel & Steinhardt 2000), as well as to interactions between baryonic and dark components (e.g. Blumenthal et al. 1986).”
BackgroundPossible Imprints of Cold-mode Accretion on the Present-day Properties of Disk Galaxies
Noguchi, M. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaa484 · Cited by 8
“This shock-heating paradigm (sometimes called “hot-mode accretion”) has been employed with considerable success in attempts to obtain a unified picture of the formation of galaxies and clusters of galaxies (e.g., Blumenthal et al. 1986; Kauffmann et al. 1993; Cole et al. 1994; Benson et al. 2003).”
MethodOn the Dwarf Galaxy Rotation Curve Diversity Problem
Popolo, A. D., Delliou, M. L., & Lee, X.-G. (2018) · Galaxies · doi:10.3390/galaxies6030067 · Cited by 8
“) The baryons collapse compresses DM (adiabatic compression), steepening the DM profile [92,93,95].”
BackgroundTwo-phase galaxy formation: the evolutionary properties of galaxies
Cook, M. J., Barausse, E., Evoli, C., et al. (2010) · Cited by 8
The Dark Halo of NGC 5963 as a Constraint on Dark Matter Self-Interaction at the Low Velocity Regime
Sánchez-Salcedo, F. J. (2005) · CERN Document Server (European Organization for Nuclear Research) · Cited by 8
Beyond mass: detecting secondary halo properties with galaxy-galaxy lensing
Xhakaj, E., Leauthaud, A., Lange, J., Hearin, A. P., Diemer, B., & Dalal, N. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac941 · Cited by 8
Not So Dark, Not So Dense: An Alternative Explanation for the Lensing Subhalo in SDSS J0946+1006
He, Q., Robertson, A., Nightingale, J. W., Amvrosiadis, A., Cole, S., Frenk, C. S., Lange, S. C., Li, S. Z., Li, R., Cao, X., et al. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ae072d · Cited by 7
Baryonification: an alternative to hydrodynamical simulations for cosmological studies
Schneider, A., Kovač, M., Bucko, J., Nicola, A., Reischke, R., Giri, S., Teyssier, R., Tröster, T., Réfrégier, A., Schaller, M., et al. (2025) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2025/12/043 · Cited by 14
“It turns out that by completely abandoning the functional form introduced by [59], it is possible to obtain a simpler empirical function that does not rely on any iterative process, returning nearly identical results than Eq.”
InfluentialTHE ENTIRE VIRIAL RADIUS OF THE FOSSIL CLUSTER RXJ 1159 + 5531. II. DARK MATTER AND BARYON FRACTION
Buote, D. A., Su, Y., Gastaldello, F., et al. (2016) · eScholarship (California Digital Library) · Cited by 7
Castro, T., Borgani, S., Costanzi, M., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202348388 · Cited by 7
The Stellar Bar–Dark Matter Halo Connection in the TNG50 Simulations
Ansar, S., & Das, M. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad7a6b · Cited by 7
“…the process, which results from two phenomena — 1. an increase in DM mass within the volume ( r m = 10 kpc), which maybe due to adiabatic contraction (Blumenthal et al. 1986; Kazantzidis et al. 2004; Gnedin et al. 2004) and 2. the transfer of angular momentum from the bar region to the DM halo.”
BackgroundAn analytical approach to the dwarf galaxies cusp problem
de Souza, R. S., & Ishida, É. E. O. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201015330 · Cited by 7
“Beyond Send offprint requests to: Rafael S. de Souza e-mail: rafael.desouza@ipmu.jp that, baryon accretion in the center of the halo will suffer adiabatic contraction and drag the dark matter profile into an even steeper one (Blumenthal et al. 1986).”
BackgroundConstraints on a nonthermal history from Galactic dark matter spikes
Sandick, P., & Watson, S. (2011) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.84.023507 · Cited by 7
Chae, K., Kravtsov, A. V., Frieman, J. A., & Bernardi, M. (2012) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2012/11/004 · Cited by 7
“Traditionally, adiabatic contraction has been invoked for the response of halos to dissipational baryonic processes [24, 25, 39, 40].”
BackgroundThe Fundamental Plane of evolving red nuggets
Oldham, L., Auger, M. W., Fassnacht, C. D., Treu, T., Koopmans, L. V. E., Lagattuta, D. J., McKean, J. P., & Vegetti, S. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx1127 · Cited by 7
“…should modify the halo in c© 2016 RAS, MNRAS 000, 000–000 some way – either contracting the halo via adiabatic processes, creating a super-NFW cusp ξ > 1 (Blumenthal et al. 1986; Gnedin et al. 2004), or hollowing it out via heating from active galactic nuclei or dynamical friction, leading to a…”
BackgroundAnalytic Approximations for the Velocity Suppression of Dark Matter Capture
Ilie, C., & Paulin, J. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac651b · Cited by 7
“Including the effects of the adiabatic compression (Young 1980; Blumenthal et al. 1986; Freese et al. 2009; Gnedin et al. 2011) on the DM-density profile would not much affect this value, since the mass enclosed within the scale radius will stay roughly constant, as the adiabatic compression…”
BackgroundMethodInfluentialCosmological Structure Formation
Primack, J. R. (2017) · Cambridge University Press eBooks · doi:10.1017/9781316535783.008 · Cited by 26
Self-citationBarkana, R., & Loeb, A. (2010) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.16587.x · Cited by 7
“Using the simple model of adiabatic compression (Blumenthal et al. 1986), they estimated that the observed 3D mass within the Einstein radius can be obtained if gas cooling increases the enclosed baryonic fraction within this radius to ∼1/3, twice the cosmic baryon fraction.”
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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