Cosmological simulations with scale-free initial conditions. I. Adiabatic hydrodynamics
dc.contributor.author | Owen, J. M. | en_US |
dc.contributor.author | Weinberg, David H. | en_US |
dc.contributor.author | Evrard, August E. | en_US |
dc.contributor.author | Hernquist, L. | en_US |
dc.contributor.author | Katz, N. | en_US |
dc.date.accessioned | 2008-08-14T19:10:29Z | |
dc.date.available | 2008-08-14T19:10:29Z | |
dc.date.issued | 1998-08-10 | en_US |
dc.identifier.citation | Owen, JM; Weinberg, DH; Evrard, AE; Hernquist, L; Katz, N. (1998). Astrophysical Journal, 503:(1, Part1) 16-36. <http://hdl.handle.net/2027.42/60581> | en_US |
dc.identifier.issn | 0004-637X | en_US |
dc.identifier.uri | http://arxiv.org/abs/astro-ph/9705109 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/60581 | |
dc.description.abstract | We analyze hierarchical structure formation based on scale-free initial conditions in an Einstein-de Sitter universe, including a baryonic component with Omega(bary) = 0.05. We present three independent, smoothed particle hydrodynamics (SPH) simulations, performed at two resolutions (32(3) and 64(3) dark matter and baryonic particles) and with two different SPH codes (TreeSPH and P3MSPH). Each simulation is based on identical initial conditions, which consist of Gaussian-distributed initial density fluctuations that have a power spectrum P(k) proportional to k(-1). The baryonic material is modeled as an ideal gas subject only to shock heating and adiabatic heating and cooling; radiative cooling and photoionization heating are not included. The evolution is expected to be self-similar in time, and under certain restrictions we identify the expected scalings for many properties of the distribution of collapsed objects in all three realizations. The distributions of dark matter masses, baryon masses, and mass- and emission-weighted temperatures scale quite reliably. However, the density estimates in the central regions of these structures are determined by the degree of numerical resolution. As a result, mean gas densities and Bremsstrahlung luminosities obey the expected scalings only when calculated within a limited dynamic range in density contrast. The temperatures and luminosities of the groups show tight correlations with the baryon masses, which we find can be well represented by power laws. The Press-Schechter (PS) approximation predicts the distribution of group dark matter and baryon masses fairly well, though it tends to overestimate the baryon masses. Combining the PS mass distribution with the measured relations for T(M) and L(M) predicts the temperature and luminosity distributions fairly accurately, though there are some discrepancies at high temperatures/luminosities. In general the three simulations agree well for the properties of resolved groups, where a group is considered resolved if it contains more than 32 particles. | en_US |
dc.format.extent | 1057104 bytes | |
dc.format.extent | 18 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.publisher | Univ Chicago Press | en_US |
dc.subject | Cosmology : Theory | en_US |
dc.subject | Hydrodynamics | en_US |
dc.subject | Large-scale Structure of Universe | en_US |
dc.subject | Methods : Numerical | en_US |
dc.title | Cosmological simulations with scale-free initial conditions. I. Adiabatic hydrodynamics | en_US |
dc.type | Article | en_US |
dc.subject.hlbsecondlevel | Physics | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.contributor.affiliationum | Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA | en_US |
dc.contributor.affiliationother | Univ Calif Lawrence Livermore Natl Lab, Livermore, CA 94551 USA | en_US |
dc.contributor.affiliationother | Ohio State Univ, Dept Astron, Columbus, OH 43210 USA | en_US |
dc.contributor.affiliationother | Univ Calif Santa Cruz, Lick Observ, Santa Cruz, CA 95064 USA | en_US |
dc.contributor.affiliationother | Univ Massachusetts, Dept Phys & Astron, Amherst, MA 01003 USA | en_US |
dc.contributor.affiliationother | Inst Astrophys, F-75014 Paris, France | en_US |
dc.contributor.affiliationumcampus | Ann Arbor | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/60581/1/Owen1997Cosmological.pdf | |
dc.identifier.doi | http://dx.doi.org/10.1086/305957 | en_US |
dc.owningcollname | Astrophysics (Physics, Department of) |
Files in this item
Remediation of Harmful Language
The University of Michigan Library aims to describe library materials in a way that respects the people and communities who create, use, and are represented in our collections. Report harmful or offensive language in catalog records, finding aids, or elsewhere in our collections anonymously through our metadata feedback form. More information at Remediation of Harmful Language.
Accessibility
If you are unable to use this file in its current format, please select the Contact Us link and we can modify it to make it more accessible to you.