Simulating the formation of cosmic structure

Frenk, Carlos S.

doi:10.1098/rsta.2002.0995

Cited by 12 publications

(6 citation statements)

References 69 publications

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“…More extensive reviews of the cold dark matter cosmological model can be found in, for example, Narlikar and Padmanabhan (2001), Frenk (2002) and Bertone et al (2005).…”

Section: Background Materialsmentioning

confidence: 99%

Galaxy formation theory

2010

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a b s t r a c tWe review the current theory of how galaxies form within the cosmological framework provided by the cold dark matter paradigm for structure formation. Beginning with the pre-galactic evolution of baryonic material we describe the analytical and numerical understanding of how baryons condense into galaxies, what determines the structure of those galaxies and how internal and external processes (including star formation, merging, active galactic nuclei, etc.) determine their gross properties and evolution. Throughout, we highlight successes and failures of current galaxy formation theory. We include a review of computational implementations of galaxy formation theory and assess their ability to provide reliable modeling of this complex phenomenon. We finish with a discussion of several ''hot topics'' in contemporary galaxy formation theory and assess future directions for this field.

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“…More extensive reviews of the cold dark matter cosmological model can be found in, for example, Narlikar and Padmanabhan (2001), Frenk (2002) and Bertone et al (2005).…”

Section: Background Materialsmentioning

confidence: 99%

Galaxy formation theory

2010

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“…The properties of dark matter haloes in the context of the LCDM paradigm have been studied in detail using numerical simulations over the past couple of decades with increasing resolution (e.g. Davis et al 1985; Efstathiou et al 1988; Frenk et al 1988; Katz, Hernquist & Weinberg 1999; Kauffmann et al 1999; Bullock et al 2001b; Frenk 2002; Springel et al 2005). This approach has been very fruitful in providing us with a detailed picture of the assembly and growth of structure in the Universe.…”

Section: Introductionmentioning

confidence: 99%

Spin and structural halo properties at high redshift in a Λ cold dark matter universe

Davis¹,

Natarajan²

2010

Monthly Notices of the Royal Astronomical Society

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In this paper, we examine in detail the key structural properties of high‐redshift dark matter haloes as a function of their spin parameter. We perform and analyse high‐resolution cosmological simulations of the formation of structure in a Λ cold dark matter universe. We study the mass function, shapes, density profiles and rotation curves for a large sample of dark matter haloes from z= 15 to 6. We also present detailed convergence tests for individual haloes. We find that high‐spin haloes have stronger clustering strengths (up to 25 per cent) at all mass and redshift ranges at these early epochs. High‐redshift spherical haloes are also up to 50 per cent more clustered than extremely aspherical haloes. High‐spin haloes at these redshifts are also preferentially found in high‐density environments, and have more neighbours than their low‐spin counterparts. We report a systematic offset in the peak of the circular velocity curves for high‐ and low‐spin haloes of the same mass. Therefore, estimating halo masses without knowledge of the spin, using only the circular velocity can yield errors of up to 40 per cent. The significant dependence of key structural properties on spin that we report here likely has important implications for studies of star formation and feedback from these galaxies.

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“…Since cdm is supposed to be electrically neutral, it is not linked by Coulomb interactions to the baryon-photon fluid. Therefore, researchers [8,9] in the field of structure formation have assumed in their simulations that cdm would have already clustered before decoupling and thus would have formed seeds for baryon contraction after decoupling. If this would be true, then the slow growth (2) would be sufficient to explain structure in the universe.…”

Section: A Former Results: Standard Perturbation Theorymentioning

confidence: 99%

Formation of Population III Stars in a flat FLRW Universe

Miedema

2010

Preprint

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Contrarily to general believe, a first-order cosmological perturbation theory based on Einstein's General Theory of Relativity explains the formation of massive primeval stars in a flat Friedmann-Lemaître-Robertson-Walker universe after decoupling of matter and radiation, whether or not Cold Dark Matter is present. The growth rate of a density perturbation depends on the heat loss of a perturbation during the contraction, but is independent of the particle mass. The relativistic Jeans mass does depend on the particle mass. If the Cold Dark Matter particle mass is equal to the proton mass, then the relativistic Jeans mass is equal to 3500 solar masses, whereas the classical Jeans mass is a factor 145 larger.

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Simulating the formation of cosmic structure

Cited by 12 publications

References 69 publications

Galaxy formation theory

Galaxy formation theory

Spin and structural halo properties at high redshift in a Λ cold dark matter universe

Formation of Population III Stars in a flat FLRW Universe

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