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Dynamics of cooling gas in galactic dark halos
Abstract
The dynamical evolution of both collisionless 'dark' particles and a dissipative gaseous component in a flat universe is simulated in order to investigate the formation process of the luminous components of galaxies at the center of galactic dark halos. The present models assume that the gas amounts to 10 percent of the mass of the universe, and that both the gas and the dark matter are identically distributed in phase space at high redshifts. The results confirm previous suggestions that the merging history of the surrounding halo is a key factor in the determination of a galaxy's morphological type. The baryonic component is found to lose more angular momentum than could be predicted by dissipationless simulations. The formation of dense, slowly rotating baryonic cores at the center of galactic dark halos is observed, which explains the origin of the slow rotation and large densities observed in spheroids and elliptical galaxies.
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Cited by
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Naab, T., & Ostriker, J. P. (2017) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081913-040019 · Cited by 722
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Stinson, G. S., Brook, C., Macciò, A. V., Wadsley, J., Quinn, T. R., & Couchman, H. M. P. (2013) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/sts028 · Cited by 431
Metadata
- Authors
- Navarro, J. F., & Benz, W.
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 1991-10
- Volume
- 380
- Pages
- 320
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2027547158
- Cited by
- 235
- References
- 0
- FWCI
- 0.72
- Type
- journal article
- Language
- en
- Open access
- closed
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