The DOI matches its Crossref record; 7 of the 7 references it cites were found in a registry or an index.
Forming disc galaxies in CDM simulations
Open accessAbstract
We used fully cosmological, high-resolution N-body + smooth particle hydrodynamic (SPH) simulations to follow the formation of disc galaxies with rotational velocities between 135 and 270 km s−1 in a Λ cold dark matter (CDM) universe. The simulations include gas cooling, star formation, the effects of a uniform ultraviolet (UV) background and a physically motivated description of feedback from supernovae (SNe). The host dark matter haloes have a spin and last major merger redshift typical of galaxy-sized haloes as measured in recent large-scale N-body simulations. The simulated galaxies form rotationally supported discs with realistic exponential scalelengths and fall on both the I band and baryonic Tully–Fisher relations. An extended stellar disc forms inside the Milky Way (MW)-sized halo immediately after the last major merger. The combination of UV background and SN feedback drastically reduces the number of visible satellites orbiting inside a MW-sized halo, bringing it in fair agreement with observations. Our simulations predict that the average age of a primary galaxy's stellar population decreases with mass, because feedback delays star formation in less massive galaxies. Galaxies have stellar masses and current star formation rates as a function of total mass that are in good agreement with observational data. We discuss how both high mass and force resolution and a realistic description of star formation and feedback are important ingredients to match the observed properties of galaxies.
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Core condensation in heavy halos: a two-stage theory for galaxy formation and clustering
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The statistics of peaks of Gaussian random fields
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“In our algorithm the time-scale for the cooling shut off and the amount of mass affected are physically motivated and chosen following typical values from the McKee & Ostriker (1977) and Ostriker & McKee (1988) blast wave model.”
MethodOstriker, J. P., & McKee, C. F. (1988) · Reviews of Modern Physics · doi:10.1103/revmodphys.60.1 · Cited by 436
Deciphering the Last Major Invasion of the Milky Way
Gilmore, G., Wyse, R. F. G., & Norris, J. E. (2002) · The Astrophysical Journal · doi:10.1086/342363 · Cited by 203
Cited by
Physical Models of Galaxy Formation in a Cosmological Framework
Somerville, R. S., & Davé, R. (2015) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-082812-140951 · Cited by 1,442
Bulgeless dwarf galaxies and dark matter cores from supernova-driven outflows
Governato, F., Brook, C., Mayer, L., Brooks, A., Rhee, G., Wadsley, J., Jonsson, P., Willman, B., Stinson, G., Quinn, T., et al. (2010) · Nature · doi:10.1038/nature08640 · Cited by 1,042
Self-citationAMAZE: I. The evolution of the mass–metallicity relation at z > 3
Maiolino, R., Nagao, T., Grazian, A., Cocchia, F., Marconi, A., Mannucci, F., Cimatti, A., Pipino, A., Ballero, S., Calura, F., et al. (2008) · Astronomy & Astrophysics · doi:10.1051/0004-6361:200809678 · Cited by 987
Theoretical Challenges in Galaxy Formation
Naab, T., & Ostriker, J. P. (2017) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081913-040019 · Cited by 722
Governato, F., Zolotov, A., Pontzen, A., Christensen, C., Oh, S. H., Brooks, A. M., Quinn, T., Shen, S., & Wadsley, J. (2012) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2012.20696.x · Cited by 640
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Metadata
- Authors
- Governato, F., Willman, B., Mayer, L., Brooks, A., Stinson, G., Valenzuela, O., Wadsley, J., & Quinn, T.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2007-02-01
- Volume
- 374
- Issue
- 4
- Pages
- 1479-1494
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2132579896
- Cited by
- 597
- References
- 7
- FWCI
- 29.89
- Type
- journal article
- Language
- en
- Open access
- bronze
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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).
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