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Author: Publisher: ISBN: Category : Languages : en Pages :
Book Description
The N Body Shop Group of the University of Washington presents information about dark matter simulations. The group provides access to an image of a final state of a dark mater simulation a movie of a rotation about the z axis, and a movie of a halo collapse.
Author: Publisher: ISBN: Category : Languages : en Pages :
Book Description
The N Body Shop Group of the University of Washington presents information about dark matter simulations. The group provides access to an image of a final state of a dark mater simulation a movie of a rotation about the z axis, and a movie of a halo collapse.
Author: Avishai Dekel Publisher: Cambridge University Press ISBN: 9780521586320 Category : Science Languages : en Pages : 492
Book Description
This advanced textbook provides an up-to-date and comprehensive introduction to the very active field of structure formation in cosmology. It is written by eleven world-leading authorities. Written in a clear and pedagogical style appropriate for graduate students in astronomy and physics, this textbook introduces the reader to a wide range of exciting topics in contemporary cosmology: from recent advances in redshift surveys, to the latest models in gravitational lensing and cosmological simulations. The authors are all world-renowned experts both for their research and teaching skills. In the fast-moving field of structure formation, this book provides advanced undergraduate and graduate students with a welcome textbook which unites the latest theory and observations.
Author: Rouven Essig Publisher: Springer Nature ISBN: 3030315932 Category : Science Languages : en Pages : 168
Book Description
Based on a Simons Symposium held in 2018, the proceedings in this volume focus on the theoretical, numerical, and observational quest for dark matter in the universe. Present ground-based and satellite searches have so far severely constrained the long-proposed theoretical models for dark matter. Nevertheless, there is continuously growing astrophysical and cosmological evidence for its existence. To address present and future developments in the field, novel ideas, theories, and approaches are called for. The symposium gathered together a new generation of experts pursuing innovative, more complex theories of dark matter than previously considered.This is being done hand in hand with experts in numerical astrophysical simulations and observational techniques—all paramount for deciphering the nature of dark matter. The proceedings volume provides coverage of the most advanced stage of understanding dark matter in various new frameworks. The collection will be useful for graduate students, postdocs, and investigators interested in cutting-edge research on one of the biggest mysteries of our universe.
Author: Oliver D. Elbert Publisher: ISBN: 9780355311112 Category : Languages : en Pages : 111
Book Description
Dark Matter (DM) accounts for the vast majority of mass in the universe, but the particle identity of dark matter remains a mystery. Uncovering the fundamental nature of DM remains one of the greatest challenges facing modern physics. Because the only information about DM comes from astrophysical observations, these are the best sources to constrain models. Dwarf galaxies present an especially tantalizing regime to investigate dark physics, as they have the highest ratio of dark to luminous matter and therefore will be most affected by differences between DM models. Additionally, this is precisely the scale where generic dark matter theories have the most difficulty reproducing astronomical observations, leading to the missing satellites, core-cusp and too-big-to-fail (TBTF) problems.A particular class of models with nuclear scale self-interactions (called SIDM) has emerged as a promising candidate. SIDM naturally forms cored halos, which may alleviate both the core-cusp and TBTF problems. However, at larger scales the the interplay between SIDM halos and the galaxies residing in them is poorly understood, complicating this picture greatly. In this thesis I present numerical simulations of SIDM and CDM halos investigating these issues. I show that at dwarf scales SIDM cross sections as small as 0.5cm2 g--1 solve the TBTF and core-cusp problems, and that cross sections 2 orders of magnitude larger are not ruled out. I have also embedded gravitational potentials that approximate realistic galaxies in simulations of larger haloes in order to test the impact of galaxy formation on SIDM halos. These simulations show that SIDM is indistinguishable from CDM in systems where the galaxy dominates the central region, but in galaxies with higher mass-to-light ratios or less centrally concentrated baryons it is possible to constrain SIDM cross sections. In the galaxy cluster regime I show that an SIDM cross section of $0.1-0.2 cm2 g --1 is preferred to CDM or other SIDM cross sections.
Author: Gianfranco Bertone Publisher: Cambridge University Press ISBN: 1139484982 Category : Science Languages : en Pages : 763
Book Description
Dark matter is among the most important open problems in modern physics. Aimed at graduate students and researchers, this book describes the theoretical and experimental aspects of the dark matter problem in particle physics, astrophysics and cosmology. Featuring contributions from 48 leading theorists and experimentalists, it presents many aspects, from astrophysical observations to particle physics candidates, and from the prospects for detection at colliders to direct and indirect searches. The book introduces observational evidence for dark matter along with a detailed discussion of the state-of-the-art of numerical simulations and alternative explanations in terms of modified gravity. It then moves on to the candidates arising from theories beyond the Standard Model of particle physics, and to the prospects for detection at accelerators. It concludes by looking at direct and indirect dark matter searches, and the prospects for detecting the particle nature of dark matter with astrophysical experiments.
Author: Società italiana di fisica Publisher: IOS Press ISBN: 1614992177 Category : Science Languages : en Pages : 739
Book Description
Physics and astrophysics came to dark matter through many different routes, finally accepting it, but often with some distaste. It has been noticed that the existence of dark matter is yet another displacement of humans from the centre of the Universe: not only do our planet and our sun have no central position in the Universe, not only are humans just animals (although with a 'specialized' central nervous system), but even the material of which we are made is only a marginal component of the cosmic substance! If this is the right attitude to take, scientists feeling distaste for dark matter are much like Galileo Galilei's colleagues who refused to look through the telescope to watch the Medici planets. Nevertheless, astronomers, when required to take a ballot in favour of some cosmological model, often still vote for 'pure baryonic' with substantial majorities, although most cosmologists assume that a 'cold' component of dark matter plays a role in producing the world as we observe it. Among the many subjects covered by the book, particular emphasis was given to 1) summarizing the current status of the observations both of the distribution of the nearby galaxies and of the evolution of more distant galaxies; 2) advanced statistical techniques for quantifying structure in galaxy redshift and peculiar velocity surveys; 3) the art of cosmic inflation and models for dark matter candidates, and their implications for cosmic microwave background observations; 4) implications of cold dark matter variants for large scale structure, as worked out both by quasi-linear techniques and by fully nonlinear simulations; and 5) Eulerian and Lagrangian approximations for treating the nonlinear dynamics.
Author: Elise Jennings Publisher: Springer Science & Business Media ISBN: 3642293395 Category : Science Languages : en Pages : 117
Book Description
A major outstanding problem in physics is understanding the nature of the dark energy that is driving the accelerating expansion of the Universe. This thesis makes a significant contribution by demonstrating, for the first time, using state-of-the-art computer simulations, that the interpretation of future galaxy survey measurements is far more subtle than is widely assumed, and that a major revision to our models of these effects is urgently needed. The work contained in the thesis was used by the WiggleZ dark energy survey to measure the growth rate of cosmic structure in 2011 and had a direct impact on the design of the surveys to be conducted by the European Space Agency's Euclid mission, a 650 million euro project to measure dark energy.
Author: Carlos Chover Lopez Publisher: ISBN: Category : Languages : en Pages :
Book Description
In the last century, new observational techniques and discoveries such as the Cosmic Microwave Background Radiation have brought a new dimension of knowledge about the Universe. Therefore new theories and models have been proposed to explain the observed Universe. Computer simulations are a very important tool because they lay a bridge between theory, often over-simpli ed, and observations, which reveal the complexity of our Universe. In this thesis, it is given a review of observations including the most important discoveries and results that help to describe the Universe and have been used to develop the models considered nowadays. The cosmological theory behind the large-scale structure formation is explained, from the basis of the Friedman model to the formation of structures through the linear, quasi-linear and non-linear regime, including the Zeldovich approximation and the spherical collapse model. Furthermore, the di erent types of codes used for cosmological simulations are introduced, focusing on the N-body codes and presenting the code used in this thesis, developed by Klypin & Holtzman (1997). The tools used to analyse the results: density plots, power spectrum and mass variance are described as well. Three main sets of simulations have been performed: a basic simulation (RUN0) with standard cosmological parameters, simulations of CDM and simulations of Hot+Cold Dark Matter (HCDM). All the simulations use 323 particles, while di erent cosmological parameters have been changed e.g. 8, m, and n. Thus, it is observed that higher values of m and low values of lead to more clustering and hence more developed structures. Moreover, the e ect of 8 appears to be critical, since it determines the amplitude of the density uctuations at the initial redshift of the simulation. When studying the presence of hot dark matter, the main di erence comes from the cut-o in the power spectrum due to the hot dark matter free-streaming, resulting in less developed structures. Similarly to the previous case, the e ects of the cosmological parameters are explained for this model. Finally, some additional simulations regarding dark halos populations and density pro- les are included in the Appendix.
Author: Philip Edward Bett Publisher: ISBN: Category : Dark matter (Astronomy) Languages : en Pages :
Book Description
We study the angular momentum, shape and density structures of dark matter haloes using very large dark matter simulations, and use smaller, higher-resolution simulations to investigate how the distributions of these properties are changed by the physical processes associated with baryons and galaxy formation. We begin with a brief review of the necessary background theory, including the growth of cosmic structures, the origin of their angular momenta, and the techniques used to simulate galaxies, haloes and the large scale structure. In Chapter 2, we use the Millennium Simulation (MS) to investigate the distributions of the spin and shape parameters of millions of dark matter haloes. We compare results for haloes identified using three different algorithms, including one based on the branches of the halo merger trees. In addition to characterising the relationships between halo spin, shape and mass, we also study their impact on halo clustering and bias. We go on in Chapter 3 to investigate the internal angular momentum structure of dark matter haloes. We look at the radial profiles of the dark matter angular momentum in terms of both magnitude and direction, again using large-volume dark matter simulations including the MS. We then directly compare dark matter haloes simulated both with and without baryonic physics, studying how this changes the dark matter angular momentum. After relating the spin orientation of galaxies to their haloes, we consider the shape of the projected, stacked mass distribution of haloes oriented according to their central galaxy, mimicking attempts to measure halo ellipticity by weak gravitational lensing. We consider the density structure of dark matter haloes in Chapter 4. For the dark matter simulations, we focus our interest on the source of the scatter in the distribution of concentration parameters, correlating it with both the halo spin and formation time. We compare different algorithms for predicting the concentration distribution using different aspects of the merger histories. We again go on to directly compare high-resolution haloes in simulations run with and without baryons and galaxy formation, looking at how these additional physical processes transform the density profiles. Finally, we compare the circular velocity curves of the haloes simulated with galaxies to the rotation curves of observed galaxies, using the Universal Rotation Curve model.
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Author: Avishai Dekel
Author: Darren S. Reed
Author: Rouven Essig
Author: Oliver D. Elbert
Author: Gianfranco Bertone
Author: Società italiana di fisica
Author: Elise Jennings
Author: Carlos Chover Lopez
Author: Philip Edward Bett