Statistical Properties of X-Ray Clusters: Analytic and Numerical Comparisons
We compare the results of Eulerian hydrodynamic simulations of cluster formation against virial scaling relations between four bulk quantities: the cluster mass, the dark matter velocity dispersion,…
The Formation of the First Star in the Universe
It is concluded that at most one massive metal-free star forms per pregalactic halo, consistent with recent abundance measurements of metal-poor galactic halo stars.
Baryons in the Warm-Hot Intergalactic Medium
Approximately 30%-40% of all baryons in the present-day universe reside in a warm-hot intergalactic medium (WHIM), with temperatures in the range 105 < T < 107 K. This is a generic prediction from…
The Santa Barbara Cluster Comparison Project: A Comparison of Cosmological Hydrodynamics Solutions
We have simulated the formation of an X-ray cluster in a cold dark matter universe using 12 different codes. The codes span the range of numerical techniques and implementations currently in use,…
The baseline intracluster entropy profile from gravitational structure formation
The radial entropy profile of the hot gas in clusters of galaxies tends to follow a power law in radius outside of the cluster core. Here we present a simple formula giving both the normalization and…
Simulations of Pregalactic Structure Formation with Radiative Feedback
- M. Machacek, G. Bryan, T. Abel
- Physics
- 14 July 2000
We present results from three-dimensional hydrodynamic simulations of the high-redshift collapse of pregalactic clouds including feedback effects from a soft H2 photodissociating UV radiation field.…
ENZO: AN ADAPTIVE MESH REFINEMENT CODE FOR ASTROPHYSICS
- Corey Brummel-Smith, G. Bryan, Fen Zhao
- PhysicsJournal of Open Source Software
- 8 July 2013
This paper describes the open-source code Enzo, which uses block-structured adaptive mesh refinement to provide high spatial and temporal resolution for modeling astrophysical fluid flows. The code…
Supermassive black hole formation by direct collapse: keeping protogalactic gas H2 free in dark matter haloes with virial temperatures Tvir > rsim 104 K
In the absence of H 2 molecules, the primordial gas in early dark matter haloes with virial temperatures just above T vir ≳ 10 4 K cools by collisional excitation of atomic H. Although it cools…
MAGNETIC FIELDS IN POPULATION III STAR FORMATION
We study the buildup of magnetic fields during the formation of Population III star-forming regions by conducting cosmological simulations from realistic initial conditions and varying the Jeans…
A Universal Temperature Profile for Galaxy Clusters
We investigate the predicted present-day temperature profiles of the hot, X-ray-emitting gas in galaxy clusters for two cosmological models—a current best-guess ΛCDM model and a standard cold dark…
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