Structure Formation in the Universe

By Enrique Gaztañaga. 2003

517 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b555c8dbc2c266439776cd6047a2aadba06e7e9b

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Citations in the corpus

Evolving turbulence and magnetic fields in galaxy clusters (2005, background): “For example, consider subclusters predicted by the hierarchical theory of structure formation (Peebles 1980; Padmanabhan & Subramanian 19 92; Padmanabhan 1993).”
Ram-pressure stripping of halo gas in disc galaxies: implications for galactic star formation in different environments (2009, methodology): “Considering virial velocities (vvir) of dark matter halos (NFW95) and the scaling relation between masses and sizes for dark matter halos (e.g., Padmanabhan 1993), reasonable values of TIGM and Vr are chosen for the above four models with different Mhost.”
Cosmological constraints on f(R) gravity theories within the Palatini approach (2005, methodology): “Although the spherical collapse model has been set and used for a long time (Peebles 1993; Padmanabhan 1993 ) and in many different contexts (Lue et al. 2004a; Mota & Barrow 2004a,b; Mota & van de Bruck 2004; Clifton et al. 2005), it has not been applied previously to Nonlinear Gravity Theories.”
Issues in the Philosophy of Cosmology (2006, background): “Observational cosmology [114, 128, 99, 189, 18] aims to determine the large-scale geometry of the observable universe and the distribution of matter in it from observations of radiation emitted by distant objects, while physical cosmology [163, 193, 233, 202, 171, 38] is the study of interactions du”
Bulk viscosity driving the acceleration of the Universe (2005, methodology): “Following [25], we adopt B = (24 hMpc)(4).”
The Formation of the First Stars. I. The Primordial Star-forming Cloud (2001, unknown): “…Yoneyama 1972 ; Hutchins 1976 ; Silk 1977, 1983 ; Carlberg 1981 ; Kashlinsky & Rees 1983 ; Palla, Salpeter, & Stahler 1983 ; Carr, Bond, & Arnett 1984 ; Couchman & Rees 1986 ; Haiman, Thoul, & Loeb 1996 ; Uehara et al. 1996 ; Tegmark et al. 1997 ; Omukai & Nishi 1998 ; Nakamura & Umemura 1999).”
Further analysis of a cosmological model with quintessence and scalar dark matter (2000, background): “Since H = τ−1 and radiation dominates equation (78), h evolves as in the standard case, ḣ = Cτ [30] (for a detailed calculus with the exponential potential, see [7]), being C = const.”
The end of unified dark matter (2002, methodology): “Following the standard calculations of [17], we obtain for the relativistic analog of the Newtonian 1st order perturbation equation in Fourier space that a density fluctuation δk with wave vector k evolves as”
MODELING COLLAPSE AND ACCRETION IN TURBULENT GAS CLOUDS: IMPLEMENTATION AND COMPARISON OF SINK PARTICLES IN AMR AND SPH (2010, background): “The corresponding scheme for preserving positive states in purely hydrodynamic studies has been tested successfully in Klingenberg et al. (2007). Moreover, Duffin & Pudritz (2008) have recently developed a non-ideal MHD scheme to model ambipolar diffusion.”
Monte Carlo Simulation of Lyα Scattering and Application to Damped Lyα Systems (2002, background): “In an M ¼ 1 universe with H0 ¼ 70 km s 1 Mpc 1, the corresponding virial radius is rvir ¼ 24 kpc and the virial velocity Vvir ¼ 104 km s 1 (see, e.g., Padmanabhan 1993).”
Cosmological constant—the weight of the vacuum (2002, background): “The above analysis is valid if recombination was instantaneous; but in reality the thickness of the recombination epoch is about ∆z ≃ 80 ([222];[44], chapter 3).”
Accelerated expansion from structure formation (2006, background): “[117, 118]), and the equivalent for underdense regions (the appendix of [119] has a useful summary of both cases).”
Ground-based and Airborne Telescopes VII (2008, background): “g.(2)) derives from the growth of initial density seeds, already visible as small anisotropies in the maps of the Cosmic Microwave Background.”
Cosmic structure formation with topological defects (2001, background): “ment [134], which has measured CMB anisotropies on large angular scales and found that they are approximately constant as expected from a Harrison-Zel’dovich spectrum of initial ﬂuctuations (see e.g. [113]). 7 Since quite some time it is known, however, that topological defect diﬀer from adiabatic i”
Can Supermassive Black Holes Form in Metal-enriched High-Redshift Protogalaxies? (2008, methodology): “Dynamical Interactions and Accretion Since dust-induced fragmentation takes place at high densities, a dense protostellar cluster is expected to form (Omukai et al. 2005; Schneider et al. 2006; Clark et al. 2008).”
The pinocchio algorithm: pinpointing orbit-crossing collapsed hierarchical objects in a linear density field (2001, methodology): “…used the second-order LPT solution for the density field (Scoccimarro & Sheth 2001), or joined linear-theory predictions with Monte-Carlo methods such as the block-model (Cole & Kaiser 1988) and merging-cell model (Rodrigues & Thomas 1996; Nagashima & Gouda 1998; Lanzoni, Mamon & Guiderdoni 2000).”