Log in

Relevant bibliographies by topics / Cosmological hydrodynamics

Contents

Journal articles
Dissertations / Theses
Books
Book chapters
Conference papers

Academic literature on the topic 'Cosmological hydrodynamics'

Author: Grafiati

Published: 4 June 2021

Last updated: 1 February 2022

Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles

Select a source type:

Consult the lists of relevant articles, books, theses, conference reports, and other scholarly sources on the topic 'Cosmological hydrodynamics.'

Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.

You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.

Journal articles on the topic "Cosmological hydrodynamics"

1

Choquet‐Bruhat, Yvonne. "Cosmological Yang–Mills hydrodynamics." Journal of Mathematical Physics 33, no. 5 (May 1992): 1782–85. http://dx.doi.org/10.1063/1.529655.

Full text

APA, Harvard, Vancouver, ISO, and other styles

2

Evrard, August E. "The Advent of Cosmological Gas Dynamic Simulations." Symposium - International Astronomical Union 130 (1988): 557. http://dx.doi.org/10.1017/s0074180900136861.

Full text

Abstract:

The next move forward in simulations of cosmological structure is to include the hydrodynamics and thermal history of a gaseous component. The task is not an easy one. The dynamic range is wide in all interesting quantities (density, temperature, length-scales, time-scales, etc.). Generic initial mass distributions sampled from Gaussian random fields will, for many interesting power spectra, lead to a high degree of substructure present at all stages of the evolution. Grid-based hydrodynamic techniques currently lack the resolution necessary to evolve several levels of a clustering hierarchy simultaneously. A particle-based method known as SPH (Smoothed Particle Hydrodynamics, see Monoghan (1985) for a review) appears best suited for cosmological application. I have recently imbedded the technique into the P3M N-body code, described by Efstathiou et al. (1985) and used extensively by Efstathiou and collaborators, most recently in investigations of the cold dark matter scenario.

APA, Harvard, Vancouver, ISO, and other styles

3

Gibson, Brad K., Stéphanie Courty, Patricia Sánchez-Blázquez, Romain Teyssier, Elisa L. House, Chris B. Brook, and Daisuke Kawata. "Hydrodynamical Adaptive Mesh Refinement Simulations of Disk Galaxies." Proceedings of the International Astronomical Union 4, S254 (June 2008): 445–52. http://dx.doi.org/10.1017/s1743921308027956.

Full text

Abstract:

AbstractTo date, fully cosmological hydrodynamic disk simulations to redshift zero have only been undertaken with particle-based codes, such as GADGET, Gasoline, or GCD+. In light of the (supposed) limitations of traditional implementations of smoothed particle hydrodynamics (SPH), or at the very least, their respective idiosyncrasies, it is important to explore complementary approaches to the SPH paradigm to galaxy formation. We present the first high-resolution cosmological disk simulations to redshift zero using an adaptive mesh refinement (AMR)-based hydrodynamical code, in this case, RAMSES. We analyse the temporal and spatial evolution of the simulated stellar disks' vertical heating, velocity ellipsoids, stellar populations, vertical and radial abundance gradients (gas and stars), assembly/infall histories, warps/lopsideness, disk edges/truncations (gas and stars), ISM physics implementations, and compare and contrast these properties with our sample of cosmological SPH disks, generated with GCD+. These preliminary results are the first in our long-term Galactic Archaeology Simulation program.

APA, Harvard, Vancouver, ISO, and other styles

4

Abadi, Mario G., Diego G. Lambas, and Patricia B. Tissera. "Cosmological Simulations with Smoothed Particle Hydrodynamics." Symposium - International Astronomical Union 168 (1996): 577–78. http://dx.doi.org/10.1017/s0074180900110757.

Full text

Abstract:

We have developed and tested a code that computes the evolution of a mixed system of gas and dark matter in expanding world models. The gravitational forces are calculated with the Adaptative P3M algorithms developed by H. Couchmann, 1993. The calculation of gas forces follow the standard SPH formalism (Monaghan, 1989).

APA, Harvard, Vancouver, ISO, and other styles

5

Teyssier, R. "Cosmological hydrodynamics with adaptive mesh refinement." Astronomy & Astrophysics 385, no. 1 (April 2002): 337–64. http://dx.doi.org/10.1051/0004-6361:20011817.

Full text

APA, Harvard, Vancouver, ISO, and other styles

6

BEREZIN, V. A. "UNUSUAL HYDRODYNAMICS." International Journal of Modern Physics A 02, no. 05 (October 1987): 1591–615. http://dx.doi.org/10.1142/s0217751x87000831.

Full text

Abstract:

A method for the phenomenological description of particle production is proposed. Correspondingly modified equations of motion and energy-momentum tensor are obtained. In order to illustrate this method we reconsider from the new point of view of (i) the C-field Hoyle-Narlikar cosmology, (ii) the influence of the particle production process on metric inside the event horizon of a charged black hole and (iii) a nonsingular cosmological model.

APA, Harvard, Vancouver, ISO, and other styles

7

Martel, Hugo, and Paul R. Shapiro. "Cosmological Simulations with Adaptive Smoothed Particle Hydrodynamics." Symposium - International Astronomical Union 208 (2003): 315–22. http://dx.doi.org/10.1017/s0074180900207262.

Full text

Abstract:

We summarize the ideas that led to the Adaptive Smoothed Particle Hydrodynamics (ASPH) algorithm, with anisotropic smoothing and shock-tracking. We then identify a serious new problem for SPH simulations with shocks and radiative cooling — false cooling — and discuss a possible solution based on the shock-tracking ability of ASPH.

APA, Harvard, Vancouver, ISO, and other styles

8

Bryan, Greg L., Michael L. Norman, James M. Stone, Renyue Cen, and Jeremiah P. Ostriker. "A piecewise parabolic method for cosmological hydrodynamics." Computer Physics Communications 89, no. 1-3 (August 1995): 149–68. http://dx.doi.org/10.1016/0010-4655(94)00191-4.

Full text

APA, Harvard, Vancouver, ISO, and other styles

9

Noh, Hyerim, Jai-chan Hwang, and Chan-Gyung Park. "Cosmological hydrodynamics with relativistic pressure and velocity." Journal of Cosmology and Astroparticle Physics 2018, no. 11 (November 5, 2018): 002. http://dx.doi.org/10.1088/1475-7516/2018/11/002.

Full text

APA, Harvard, Vancouver, ISO, and other styles

10

Miller, J. C., and O. Pantano. "Hydrodynamics of the cosmological quark-hadron transition." Physical Review D 40, no. 6 (September 15, 1989): 1789–97. http://dx.doi.org/10.1103/physrevd.40.1789.

Full text

APA, Harvard, Vancouver, ISO, and other styles

More sources

Dissertations / Theses on the topic "Cosmological hydrodynamics"

1

Jubelgas, Martin. "Cosmological Hydrodynamics: Thermal Conduction and Cosmic Rays." Diss., [S.l.] : [s.n.], 2007. http://edoc.ub.uni-muenchen.de/archive/00006928.

Full text

APA, Harvard, Vancouver, ISO, and other styles

2

More, James G. "The large scale structure of the universe in pancake models of galaxy formation." Thesis, University of Edinburgh, 1989. http://hdl.handle.net/1842/28659.

Full text

Abstract:

This thesis investigates the evolution of characteristic structures in neutrino or adiabatic baryon-dominated models of galaxy formation. We discuss the collapse of protocluster or protosupercluster clouds in terms of the behaviour of non-rotating, homogeneous triaxial ellipsoids, predicting that galaxies should populate filamentary or quasi-spherical structures rather than the generic flat structures (pancakes). Secondly we have designed a numerical code which allows us to do fast cosmological hydrodynamics. We investigate the effect of explosions on the standard pancake picture for galaxy formation. Blast waves created by the early evolution of galaxies can not produce the anti-biasing effect required to reconcile the rapid evolution of clustering in n-body simulations of neutrino models with observations of galaxies at redshifts greater than one.

APA, Harvard, Vancouver, ISO, and other styles

3

Rosdahl, Karl Joakim. "Cosmological RHD simulations of early galaxy formation." Thesis, Lyon 1, 2012. http://www.theses.fr/2012LYO10075/document.

Full text

Abstract:

Avec l’essor actuel de la sophistication et de l’efficacité des codes de cosmologie hydrodynamique,il est devenu possible d’inclure le transfert radiatif (RT) des photons ionisants dansles simulations cosmologiques, soit en post-traitement, soit en simulations couplées rayonnement+hydrodynamique (RHD). Malgré de nombreux obstacles, il y a eu cette derniéredécennie beaucoup de recherches menées sur les différentes stratégies et implémentations,dû au fait qu’un nombre de problèmes intéressants peuvent être désormais abordés par laRT et RHD, par exemple comment et quand l’Univers s’est réionisé, comment l’émissionradiative des étoiles et des noyaux actifs de galaxies se comportent pour réguler la formationdes structures à des échelles petites et grandes, et quelles prédictions et interprétationsnous pouvons faire des phénomènes observés, tels que la forêt Lyman-alpha et des sourcesdiffuses de rayonnement.Cela coïncide avec l’avènement du télescope spatial James Webb (JWST) et d’autresinstruments de pointe qui sont sur le point de nous donner un aperçu sans précédent sur lafin des âges sombres de l’Univers, quand le cosmos est passé d’un état froid et neutre à unétat chaud et ionisé, à la suite de l’apparition des sources radiatives.Notre préoccupation principale étant les rétroactions radiatives des premieres structures,nous avons mis en place une version RHD du code cosmologique Ramses, que nous appelonsRamsesRT, basée sur la méthode des moments. Ce code nous permet d’étudier les effets durayonnement ionisant dans les simulations cosmologiques RHD qui tirent pleinement profitdes stratégies de raffinement adaptif de grille et de parallélisation de Ramses. Pour rendreauto-cohérent le RHD nous avons également mis en oeuvre une thermochimie hors-équilibreincluant des espèces de l’Hydrogène et de l’Hélium qui interagissent avec le rayonnementtransporté.Je présente dans cette thèse une description détaillée de RamsesRT et de nombreux testscontribuant à sa validation.Jusqu’à présent nous avons utilisé RamsesRT pour étudier l’émission Lyman-alpha decourants d’accrétion, qui sont prédits à grand redshift par les simulations cosmologiques,mais n’ont jamais été clairement identifiés par les observations. Nous avons également étudiéle chauffage gravitationnel dans ces courants pour déterminer si ce dernier pouvait être lasource motrice principale des Lyman-alpha blobs, un phénomène observé qui a été beaucoupétudié et débattu au cours de la dernière décennie. Cet étudie nous permet de conclure queles Lyman-alpha blobs peuvent, en principe, être alimentés par le chauffage gravitationnel,et que d’autre part, les courants d’accrétion sont sur le point d’être directement détectablesavec des instruments à venir.Mes intentions futures sont d’utiliser RamsesRT dans les simulations cosmologiques àhaute résolution, de la formation des premiéres galaxies jusqu’à l’époque de la réionisation,et ainsi étudier comment la rétroaction radiative affecte la formation et l’évolution de cesgalaxies et de faire des prévisions d’observation qui peuvent être testées avec des instrumentssophistiqués tels que le JWST
With the increasing sophistication and efficiency of cosmological hydrodynamics codes, ithas become viable to include ionizing radiative transfer (RT) in cosmological simulations,either in post-processing or in full-blown radiation-hydrodynamics (RHD) simulations. Inspite of the many hurdles involved, there has been much activity during the last decade or soon different strategies and implementations, because a number of interesting problems canbe addressed with RT and RHD, e.g. how and when the Universe became reionized, howradiation from stars and active galactic nuclei plays a part in regulating structure formationon small and large scales, and what predictions and interpretations we can make of observedphenomena such as the Lyman-alpha forest and diffuse sources of radiation.This coincides with the advent of the James Webb space telescope (JWST) and otherstate-of-the-art instruments which are about to give us an unprecedented glimpse into theend of the dark ages of the Universe, when the cosmos switched from a cold and neutralstate to a hot and ionized one, due to the turn-on of ionizing radiative sources.With a primary interest in the problem of radiative feedback in early structure formation,we have implemented an RHD version of the Ramses cosmological code we call RamsesRT,which is moment based and employs the local M1 Eddington tensor closure. This code allowsus to study the effects of ionizing radiation on-the-fly in cosmological RHD simulationsthat take full advantage of the adaptive mesh refinement and parallelization strategies ofRamses. For self-consistent RHD we have also implemented a non-equilibrium chemistry ofthe atomic hydrogen and helium species that interact with the transported radiation.I present in this thesis an extensive description of the RamsesRT implementation andnumerous tests to validate it.Thus far we have used the RHD implementation to study extended line emission fromaccretion streams, which are routinely predicted to exist at early redshift by cosmologicalsimulations but have never been unambiguously verified by observations, and to investigatewhether gravitational heating in those streams could be the dominant power source ofso-called Lyman-alpha blobs, an observed phenomenon which has been much studied anddebated during the last decade or two. Our conclusions from this investigation are thatLyman-alpha blobs can in principle be powered by gravitational heating, and furthermorethat accretion streams are on the verge of being directly detectable for the first time withupcoming instruments.My future intent is to use RamsesRT for high-resolution cosmological zoom simulations ofearly galaxy formation, up to the epoch of reionization, to study how radiative feedbackaffects the formation and evolution of those galaxies and to make observational predictionsthat can be tested with upcoming instruments such as the JWST

APA, Harvard, Vancouver, ISO, and other styles

4

Feng, Yu. "Petascale Cosmological Hydrodynamic Simulation of Quasars." Research Showcase @ CMU, 2014. http://repository.cmu.edu/dissertations/395.

Full text

Abstract:

This thesis presents a theoretical investigation of supermassive black holes and the quasars they power through cosmological hydrodynamic simulations on petascale supercomputers. As the size of simulations increase, visualization and interaction with the data become difficult. We developed interactive visualization software on top of existing image deep-zoom and tagging infrastructure libraries and platforms, specifically in the context of cosmological hydrodynamic simulations. The visualization tools were instrumental in establishing the cold flow fueling model of high redshift quasar growth. We then proceed to further study this growth model with high resolution zoom-in re-simulations, and report that the cold flows feeding supermassive blackholes are numerically stable. We studied the morphology of HII regions with a parallel implementation of the ray tracing scheme SPHRAY, and found that the HII regions due to high redshift quasars are smoother and more extended that those due to galaxies. Finally, we developed a set of tools to produce and verify mocked correlated quasars and Lyman-α forest. We fit the linear theory correlation function of the Quasar-Quasar and Forest-Forest auto-correlation and Quasar-Forest cross-correlation of the mocked transmission fraction and quasar locations up to 160 Mpc/h.

APA, Harvard, Vancouver, ISO, and other styles

5

Gabor, Jared. "Building a Red Sequence in Cosmological Hydrodynamic Simulations." Diss., The University of Arizona, 2011. http://hdl.handle.net/10150/202937.

Full text

Abstract:

Despite years of study, the origins of red galaxies are not fully understood in a cosmological context. We develop new models for quenching star-formation and producing red galaxies in cosmological hydrodynamic simulations. We start with phenomenological models applied in post-processing to previously-run simulations. We focus separately on mergers and hot haloes – akin to “quasar mode” and “radio mode” feedback – as the drivers shutting down star-formation. With appropriate parameter choices, each model can produce a reasonably good match observed color-magnitude diagrams and red galaxy luminosity functions at redshift zero. We uncover some difficulties with these models in general, including red galaxy stellar populations that appear too blue by 0.1 magnitudes in g − r due to a metallicity deficit. Building on the post-processing models, we develop quenching models for simulations that run on-the-fly. Again, we test merger quenching and hot halo quenching separately. We model merger feedback as > 1000 km s⁻¹ winds motivated by observations of post-starburst galaxies, and wemodel hot halo feedback by continuously adding thermal energy to circum-galactic gas in haloes dominated by gas above 250, 000 K. Merger quenching temporarily shuts down starformation, butmerger-remnant galaxies typically resume star-formation with 1− 2 Gyrs thanks to accretion of newfuel fromthe IGM.Hot halo quenching successfully produces a realistic red sequence, providing a good match to the observed red galaxy luminosity function. Despite some minor difficulties with hot halo quenching, we examine its effects in more detail. Specifically, we study the evolution of the simulated red sequence over time. We find that galaxies with stellar mass ∼ 10¹¹M⊙ are the first to populate the red sequence at z ≳ 2, with significantly fewer red galaxies around 10¹⁰M⊙ until z ≈ 0. We show that massive galaxies grow substantially after moving onto the red sequence, primarily through minor mergers. We also examine the relationship between quenching and environment.

APA, Harvard, Vancouver, ISO, and other styles

6

Owen, John Michael. "Studying cosmological structure formation with numerical hydrodynamic simulations /." The Ohio State University, 1997. http://rave.ohiolink.edu/etdc/view?acc_num=osu1487943341530188.

Full text

APA, Harvard, Vancouver, ISO, and other styles

7

Yoshikawa, Koji. "Cosmological Hydrodynamic Simulations of Galaxies and Galaxy Clusters." 京都大学 (Kyoto University), 2002. http://hdl.handle.net/2433/149981.

Full text

APA, Harvard, Vancouver, ISO, and other styles

8

Finlator, Kristian Markwart. "Comparing Cosmological Hydrodynamic Simulations with Observations of High-Redshift Galaxy Formation." Diss., The University of Arizona, 2009. http://hdl.handle.net/10150/195788.

Full text

Abstract:

We use cosmological hydrodynamic simulations to study the impact of out-flows and radiative feedback on high-redshift galaxies. For outflows, we consider simulations that assume (i) no winds, (ii) a .constant-wind. model in which the mass-loading factor and outflow speed are constant, and (iii) "momentum driven" winds in which both parameters vary smoothly with mass. In order to treat radiative feedback, we develop a moment-based radiative transfer technique that operates in both post-processing and coupled radiative hydrodynamic modes. We first ask how outflows impact the broadband spectral energy distributions (SEDs) of six observed reionization-epoch galaxies. Simulations reproduce five regardless of the outflow prescription, while the sixth suggests an unusually bursty star formation history. We conclude that (i) simulations broadly account for available constraints on reionization-epoch galaxies, (ii) individual SEDs do not constrain outflows, and (iii) SED comparisons efficiently isolate objects that challenge simulations. We next study how outflows impact the galaxy mass metallicity relation (MZR). Momentum-driven outflows uniquely reproduce observations at z = 2. In this scenario, galaxies obey two equilibria: (i) The rate at which a galaxy processes gas into stars and outflows tracks its inflow rate; and (ii) The gas enrichment rate owing to star formation balances the dilution rate owing to inflows. Combining these conditions indicates that the MZR is dominated by the (instantaneous) variation of outflows with mass, with more-massive galaxies driving less gas into outflows per unit stellar mass formed. Turning to radiative feedback, we use post-processing simulations to study the topology of reionization. Reionization begins in overdensities and then .leaks. directly into voids, with filaments reionizing last owing to their high density and low emissivity. This result conflicts with previous findings that voids ionize last. We argue that it owes to the uniqely-biased emissivity field produced by our star formation prescriptions, which have previously been shown to reproduce numerous post-reionization constraints. Finally, preliminary results from coupled radiative hydrodynamic simulations indicate that reionization suppresses the star formation rate density by at most 10.20% by z = 5. This is much less than previous estimates, which we attribute to our unique reionization topology although confirmation will have to await more detailed modeling.

APA, Harvard, Vancouver, ISO, and other styles

9

Furlong, Michelle. "A study of galaxy formation across cosmic time from cosmological hydrodynamical simulations." Thesis, Durham University, 2014. http://etheses.dur.ac.uk/10983/.

Full text

Abstract:

The evolution of galaxies across cosmic time, from the first galaxies to the local Universe, are studied using cosmological hydrodynamical simulations. It is demonstrated that, for the first time, a hydrodynamical simulation can reproduce the observed evolution of galaxy stellar masses and the trends in star formation rates. The success of the simulation in producing galaxies with similar histories to those observed increases the potential for using hydrodynamical simulations to explore galaxy formation physics. With this intention, we consider the effects of the environment and active galactic nuclei (AGN) quenching on the galaxy population and the shape of the galaxy stellar mass function (GSMF). We find environmental processes are effective at quenching galaxies in the simulation and operated on short timescales. AGN feedback, which produces a large passive fraction at high stellar masses, drives the exponential break in the GSMF. Specific star formation rates (SFRs) in simulations, both hydrodynamical and semi-analytical, have been shown to be discrepant with observations. We investigate proposed solutions to this problem using a suite of cosmological hydrodynamical simulations. The offset in the simulations, at the level of 0.2 to 0.4 dex, can only be resolved by employing an extreme model that does not recover any of the observed trends in stellar mass or the cosmic star formation rate density. This study implies that the observed star formation rates across comic time are inconsistent with the growth of stellar mass. Two galaxy populations are then explored in more detail. We examine the first galaxies and their potential to reionize the Universe. We find that low-mass galaxies, undergoing extreme star formation for their stellar mass, produce the majority of ionizing photons at redshifts 6 and above. The second study considers the most highly star forming galaxies in the simulation, which represent an extreme population. These galaxies have similar stellar and gas masses to the observed sub-mm population, however, their SFRs are lower. On further investigation, the selection of galaxies based on SFRs is not adequate to compare the simulation to the sub-mm population, in particular at high redshift. These results highlight the importance of dust temperature in the selection.

APA, Harvard, Vancouver, ISO, and other styles

10

Schaller, Matthieu. "Effects of baryons on the dark matter distribution in cosmological hydrodynamical simulations." Thesis, Durham University, 2015. http://etheses.dur.ac.uk/11275/.

Full text

Abstract:

Simulations including solely dark matter performed over the last three decades have delivered an accurate and robust description of the cosmic web and dark matter structures. With the advent of more precise cosmological probes, planned and ongoing, and dark matter detection experiments, this numerical modelling has to be improved to incorporate the complex non-linear and energetic processes taking place during galaxy formation. We use the ``Evolution and Assembly of GaLaxies and their Environment'' (EAGLE) suite of cosmological simulations to investigate the effects of baryons and astrophysical processes on the underlying dark matter distribution. Many effects are expected and we investigate (i): the modification of the profile of halos from the Navarro-Frenk-White profile shape found in collisionless simulations, including the changes in the dark matter profiles themselves, (ii) the changes of the inner density profiles of rich clusters, where observations have suggested a deviation from the standard cold dark matter paradigm, (iii) the offset created by astrophysical process between the centre of galaxies and the centre of the dark matter halo in which they reside and, (iv) the changes in the shape of the dark matter profile due to baryons in the centre of Milky Way halos and the impact these changes have on the morphology of the annihilation signal that could be observed as an indirect proof of the existence of dark matter. In all cases we find that the baryons play a significant role and change the results found in collisionless simulations dramatically. This highlights the need for more simulations like EAGLE to better understand and analyse future cosmology surveys. We also conduct a thorough study of the hydrodynamics solver parameters used in these simulations, assess their impact on the simulated galaxy population and show how robust some of the EAGLE results are against such variations.

APA, Harvard, Vancouver, ISO, and other styles

More sources

Books on the topic "Cosmological hydrodynamics"

1

Trac, Hy. Out-of-core hydrodynamic simulations of cosmological structure formation. 2004.

Find full text

APA, Harvard, Vancouver, ISO, and other styles

Book chapters on the topic "Cosmological hydrodynamics"

1

Abadi, Mario G., Diego G. Lambas, and Patricia B. Tissera. "Cosmological Simulations with Smoothed Particle Hydrodynamics." In Examining the Big Bang and Diffuse Background Radiations, 577–78. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0145-2_87.

Full text

APA, Harvard, Vancouver, ISO, and other styles

2

Nagamine, Kentaro, Renyue Cen, Lars Hernquist, Jeremiah P. Ostriker, and Volker Springel. "Massive Galaxies at Z = 2 in Cosmological Hydrodynamic Simulations." In Starbursts, 319–22. Dordrecht: Springer Netherlands, 2005. http://dx.doi.org/10.1007/1-4020-3539-x_58.

Full text

APA, Harvard, Vancouver, ISO, and other styles

3

Pfrommer, C., V. Springel, T. A. Enβlin, and M. Jubelgas. "Cosmological Structure Formation Shocks and Cosmic Rays in Hydrodynamical Simulations." In Eso Astrophysics Symposia, 371–77. Berlin, Heidelberg: Springer Berlin Heidelberg, 2007. http://dx.doi.org/10.1007/978-3-540-73484-0_68.

Full text

APA, Harvard, Vancouver, ISO, and other styles

4

da Silva, António J. C. "SZ Scaling Relations in Galaxy Clusters: Results from Hydrodynamical N-Body Simulations." In 3K, SN’s, Clusters: Hunting the Cosmological Parameters with Precision Cosmology, 167–76. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/978-94-017-0559-2_13.

Full text

APA, Harvard, Vancouver, ISO, and other styles

5

Springel, Volker, Annalisa Pillepich, Rainer Weinberger, Rüdiger Pakmor, Lars Hernquist, Dylan Nelson, Shy Genel, et al. "The Illustris++ Project: The Next Generation of Cosmological Hydrodynamical Simulations of Galaxy Formation." In High Performance Computing in Science and Engineering ´16, 5–20. Cham: Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-47066-5_1.

Full text

APA, Harvard, Vancouver, ISO, and other styles

6

"Cosmological hydrodynamics." In Relativistic Numerical Hydrodynamics, 99–116. Cambridge University Press, 2003. http://dx.doi.org/10.1017/cbo9780511615917.005.

Full text

APA, Harvard, Vancouver, ISO, and other styles

7

Dolag, Klaus. "Hydrodynamic Methods for Cosmological Simulations." In The Encyclopedia of Cosmology, 57–90. WORLD SCIENTIFIC, 2018. http://dx.doi.org/10.1142/9789813231962_0003.

Full text

APA, Harvard, Vancouver, ISO, and other styles

Conference papers on the topic "Cosmological hydrodynamics"

1

Bode, Paul W., Guohong Xu, and Renyue Cen. "A parallel cosmological hydrodynamics code." In the 1996 ACM/IEEE conference. New York, New York, USA: ACM Press, 1996. http://dx.doi.org/10.1145/369028.369085.

Full text

APA, Harvard, Vancouver, ISO, and other styles

2

Norman, Michael L., Daniel R. Reynolds, Geoffrey C. So, Ivan Hubeny, James M. Stone, Keith MacGregor, and Klaus Werner. "Cosmological Radiation Hydrodynamics with Enzo." In RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND RADIATION HYDRODYNAMICS: Proceedings of the International Conference in Honor of Dimitri Mihalas for His Lifetime Scientific Contributions on the Occasion of His 70th Birthday. AIP, 2009. http://dx.doi.org/10.1063/1.3250065.

Full text

APA, Harvard, Vancouver, ISO, and other styles

3

Meiksin, Avery, and Piero Madau. "The hydrodynamics of relict cosmological H ii regions: impact of the IGM." In After the first three minutes. AIP, 1991. http://dx.doi.org/10.1063/1.40394.

Full text

APA, Harvard, Vancouver, ISO, and other styles

4

Nagamine, Kentaro. "Galaxy formation and chemical enrichment using cosmological hydrodynamic simulations." In ORIGIN OF MATTER AND EVOLUTION OF GALAXIES 2013: Proceedings of the 12th International Symposium on Origin of Matter and Evolution of Galaxies (OMEG12). AIP Publishing LLC, 2014. http://dx.doi.org/10.1063/1.4874042.

Full text

APA, Harvard, Vancouver, ISO, and other styles

5

Oser, Ludwig, Manisha Gajbe, Kentaro Nagamine, Greg Bryan, Jeremiah P. Ostriker, and Renyue Cen. "Alleviating the scaling problem of cosmological hydrodynamic simulations with HECA." In XSEDE '13: Extreme Science and Engineering Discovery Environment: Gateway to Discovery. New York, NY, USA: ACM, 2013. http://dx.doi.org/10.1145/2484762.2484776.

Full text

APA, Harvard, Vancouver, ISO, and other styles

6

Pilkington, Kate. "The Distribution Of Metals In Cosmological Hydrodynamical Simulations Of Dwarf Disk Galaxies." In XII International Symposium on Nuclei in the Cosmos. Trieste, Italy: Sissa Medialab, 2013. http://dx.doi.org/10.22323/1.146.0227.

Full text

APA, Harvard, Vancouver, ISO, and other styles

We offer discounts on all premium plans for authors whose works are included in thematic literature selections. Contact us to get a unique promo code!