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Journal articles on the topic 'Cosmological hydrodynamics'

Author: Grafiati
Published: 4 June 2021
Last updated: 1 February 2022

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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.

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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.

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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.
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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.

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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.
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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.

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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).
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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.

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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.

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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.
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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.

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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.
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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.

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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.

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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.

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11

Gemelli, Gianluca. "Hydrodynamics in 5-Dimensional Cosmological Special Relativity." International Journal of Theoretical Physics 46, no. 5 (December 2, 2006): 1431–41. http://dx.doi.org/10.1007/s10773-006-9282-1.

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12

DIEZ-TEJEDOR, ALBERTO, and ALEXANDER FEINSTEIN. "RELATIVISTIC HYDRODYNAMICS WITH SOURCES FOR COSMOLOGICAL K-FLUIDS." International Journal of Modern Physics D 14, no. 09 (September 2005): 1561–76. http://dx.doi.org/10.1142/s0218271805007152.

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We consider hydrodynamics with non-conserved number of particles and show that it can be modeled with effective fluid Lagrangians which explicitly depend on the velocity potentials. For such theories, the "shift symmetry" ϕ → ϕ + const leading to the conserved number of fluid particles in conventional hydrodynamics is globally broken and, as a result, the non-conservation of particle number appears as a source term in the continuity equation. The non-conservation of particle number is balanced by the entropy change, with both the entropy and the source term expressed in terms of the fluid velocity potential. Equations of hydrodynamics are derived using a modified version of Schutz's variational principle method. Examples of fluids described by such Lagrangians (tachyon condensate, K-essence) in spatially flat isotropic universe are briefly discussed.
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13

Wiersma, Robert P. C., Joop Schaye, Tom Theuns, Claudio Dalla Vecchia, and Luca Tornatore. "Chemical enrichment in cosmological, smoothed particle hydrodynamics simulations." Monthly Notices of the Royal Astronomical Society 399, no. 2 (October 21, 2009): 574–600. http://dx.doi.org/10.1111/j.1365-2966.2009.15331.x.

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14

Stinson, G. S., J. Bailin, H. Couchman, J. Wadsley, S. Shen, S. Nickerson, C. Brook, and T. Quinn. "Cosmological galaxy formation simulations using smoothed particle hydrodynamics." Monthly Notices of the Royal Astronomical Society 408, no. 2 (August 25, 2010): 812–26. http://dx.doi.org/10.1111/j.1365-2966.2010.17187.x.

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15

Hwang, Jai-chan, Hyerim Noh, and Dirk Puetzfeld. "Cosmological non-linear hydrodynamics with post-Newtonian corrections." Journal of Cosmology and Astroparticle Physics 2008, no. 03 (March 12, 2008): 010. http://dx.doi.org/10.1088/1475-7516/2008/03/010.

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16

Rosdahl, J., J. Blaizot, D. Aubert, T. Stranex, and R. Teyssier. "ramses-rt: radiation hydrodynamics in the cosmological context." Monthly Notices of the Royal Astronomical Society 436, no. 3 (October 9, 2013): 2188–231. http://dx.doi.org/10.1093/mnras/stt1722.

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17

Springel, V., and L. Hernquist. "Cosmological smoothed particle hydrodynamics simulations: the entropy equation." Monthly Notices of the Royal Astronomical Society 333, no. 3 (July 1, 2002): 649–64. http://dx.doi.org/10.1046/j.1365-8711.2002.05445.x.

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18

Garecki, J., and J. Stelmach. "Cosmological implications of some parametrization of gravitating hydrodynamics." Annals of Physics 204, no. 2 (December 1990): 315–30. http://dx.doi.org/10.1016/0003-4916(90)90392-2.

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19

Shekh, S. H., Simran Arora, V. R. Chirde, and P. K. Sahoo. "Thermodynamical aspects of relativistic hydrodynamics in f(R,G) gravity." International Journal of Geometric Methods in Modern Physics 17, no. 03 (March 2020): 2050048. http://dx.doi.org/10.1142/s0219887820500486.

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We present investigation devoted to the dynamical study of relativistic hydrodynamics with some thermodynamical characteristics in [Formula: see text] gravity towards spatially homogeneous isotropic cosmological model filled with isotropic fluid. We govern the features of the derived cosmological model by considering the power-law inflation for the average scale factor. The temperature and entropy density of the proposed model are positive definite. We also discuss the energy conditions to our solutions. The strong energy condition violated, which indicates the accelerated expansion of the proposed model.
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20

Emberson, J. D., Nicholas Frontiere, Salman Habib, Katrin Heitmann, Patricia Larsen, Hal Finkel, and Adrian Pope. "The Borg Cube Simulation: Cosmological Hydrodynamics with CRK-SPH." Astrophysical Journal 877, no. 2 (May 29, 2019): 85. http://dx.doi.org/10.3847/1538-4357/ab1b31.

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21

Pfrommer, C., V. Springel, T. A. Ensslin, and M. Jubelgas. "Detecting shock waves in cosmological smoothed particle hydrodynamics simulations." Monthly Notices of the Royal Astronomical Society 367, no. 1 (March 21, 2006): 113–31. http://dx.doi.org/10.1111/j.1365-2966.2005.09953.x.

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22

Ricker, P. M., S. Dodelson, and D. Q. Lamb. "COSMOS: A HybridN‐Body/Hydrodynamics Code for Cosmological Problems." Astrophysical Journal 536, no. 1 (June 10, 2000): 122–43. http://dx.doi.org/10.1086/308908.

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23

Anninos, Wenbo Y., and Michael J. Norman. "Nonlinear hydrodynamics of cosmological sheets. 1: Numerical techniques and tests." Astrophysical Journal 429 (July 1994): 434. http://dx.doi.org/10.1086/174335.

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24

Katz, Harley, Taysun Kimm, Martin G. Haehnelt, Debora Sijacki, Joakim Rosdahl, and Jeremy Blaizot. "Tracing the sources of reionization in cosmological radiation hydrodynamics simulations." Monthly Notices of the Royal Astronomical Society 483, no. 1 (November 23, 2018): 1029–41. http://dx.doi.org/10.1093/mnras/sty3154.

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25

Simha, Vimal, David H. Weinberg, Romeel Davé, Mark Fardal, Neal Katz, and Benjamin D. Oppenheimer. "Testing subhalo abundance matching in cosmological smoothed particle hydrodynamics simulations." Monthly Notices of the Royal Astronomical Society 423, no. 4 (May 28, 2012): 3458–73. http://dx.doi.org/10.1111/j.1365-2966.2012.21142.x.

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26

Owen, J. Michael, David H. Weinberg, August E. Evrard, Lars Hernquist, and Neal Katz. "Cosmological Simulations with Scale‐Free Initial Conditions. I. Adiabatic Hydrodynamics." Astrophysical Journal 503, no. 1 (August 10, 1998): 16–36. http://dx.doi.org/10.1086/305957.

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27

Reynolds, Daniel R., John C. Hayes, Pascal Paschos, and Michael L. Norman. "Self-consistent solution of cosmological radiation-hydrodynamics and chemical ionization." Journal of Computational Physics 228, no. 18 (October 2009): 6833–54. http://dx.doi.org/10.1016/j.jcp.2009.06.006.

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28

Dai, Biwei, and Uroš Seljak. "Learning effective physical laws for generating cosmological hydrodynamics with Lagrangian deep learning." Proceedings of the National Academy of Sciences 118, no. 16 (April 14, 2021): e2020324118. http://dx.doi.org/10.1073/pnas.2020324118.

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The goal of generative models is to learn the intricate relations between the data to create new simulated data, but current approaches fail in very high dimensions. When the true data-generating process is based on physical processes, these impose symmetries and constraints, and the generative model can be created by learning an effective description of the underlying physics, which enables scaling of the generative model to very high dimensions. In this work, we propose Lagrangian deep learning (LDL) for this purpose, applying it to learn outputs of cosmological hydrodynamical simulations. The model uses layers of Lagrangian displacements of particles describing the observables to learn the effective physical laws. The displacements are modeled as the gradient of an effective potential, which explicitly satisfies the translational and rotational invariance. The total number of learned parameters is only of order 10, and they can be viewed as effective theory parameters. We combine N-body solver fast particle mesh (FastPM) with LDL and apply it to a wide range of cosmological outputs, from the dark matter to the stellar maps, gas density, and temperature. The computational cost of LDL is nearly four orders of magnitude lower than that of the full hydrodynamical simulations, yet it outperforms them at the same resolution. We achieve this with only of order 10 layers from the initial conditions to the final output, in contrast to typical cosmological simulations with thousands of time steps. This opens up the possibility of analyzing cosmological observations entirely within this framework, without the need for large dark-matter simulations.
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29

Bournaud, Frédéric. "Galaxy formation hydrodynamics: From cosmic flows to star-forming clouds." Proceedings of the International Astronomical Union 6, S270 (May 2010): 491–98. http://dx.doi.org/10.1017/s174392131100086x.

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AbstractMajor progress has been made over the last few years in understanding hydrodynamical processes on cosmological scales, in particular how galaxies get their baryons. There is increasing recognition that a large part of the baryons accrete smoothly onto galaxies, and that internal evolution processes play a major role in shaping galaxies – mergers are not necessarily the dominant process. However, predictions from the various assembly mechanisms are still in large disagreement with the observed properties of galaxies in the nearby Universe. Small-scale processes have a major impact on the global evolution of galaxies over a Hubble time and the usual sub-grid models account for them in a far too uncertain way. Understanding when, where and at which rate galaxies formed their stars becomes crucial to understand the formation of galaxy populations. I discuss recent improvements and current limitations in “resolved” modeling of star formation, aiming at explicitly capturing star-forming instabilities, in cosmological and galaxy-sized simulations. Such models need to develop three-dimensional turbulence in the ISM, which requires parsec-scale resolution at redshift zero.
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30

Anninos, Peter, Yu Zhang, Tom Abel, and Michael L. Norman. "Cosmological hydrodynamics with multi-species chemistry and nonequilibrium ionization and cooling." New Astronomy 2, no. 3 (August 1997): 209–24. http://dx.doi.org/10.1016/s1384-1076(97)00009-2.

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31

Thompson, Robert, Kentaro Nagamine, Jason Jaacks, and Jun-Hwan Choi. "MOLECULAR HYDROGEN REGULATED STAR FORMATION IN COSMOLOGICAL SMOOTHED PARTICLE HYDRODYNAMICS SIMULATIONS." Astrophysical Journal 780, no. 2 (December 19, 2013): 145. http://dx.doi.org/10.1088/0004-637x/780/2/145.

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32

Oñorbe, Jose, F. B. Davies, Z. Lukić, J. F. Hennawi, and D. Sorini. "Inhomogeneous reionization models in cosmological hydrodynamical simulations." Monthly Notices of the Royal Astronomical Society 486, no. 3 (May 4, 2019): 4075–97. http://dx.doi.org/10.1093/mnras/stz984.

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ABSTRACT In this work we present a new hybrid method to simulate the thermal effects of reionization in cosmological hydrodynamical simulations. The method improves upon the standard approach used in simulations of the intergalactic medium (IGM) and galaxy formation without a significant increase in the computational cost, thereby allowing for efficient exploration of the parameter space. The method uses a small set of phenomenological input parameters, and combines a seminumerical reionization model to solve for the topology of reionization with an approximate model of how reionization heats the IGM, using the massively parallel Nyx hydrodynamics code which is specifically designed to solve for the structure of diffuse IGM gas. We have produced several medium-scale, high-resolution simulations (20483, Lbox = 40 Mpc h−1) with various instantaneous and inhomogeneous ${\rm H \,{\small I}}$ reionization models that use this new methodology. We study the IGM thermal properties of these models and find that large-scale temperature fluctuations extend well beyond the end of reionization. By analysing the 1D flux power spectrum of these models, we find up to ${\sim } 50{{\ \rm per\ cent}}$ differences in the large-scale properties (low modes, k ≲ 0.01 s km−1) of the post-reionization power spectrum as a result of the thermal fluctuations. We show that these differences could allow one to distinguish between different reionization scenarios with existing Lyα forest measurements. Finally, we explore the differences in the small-scale cut-off of the power spectrum, finding that, for the same heat input, models show very good agreement provided that the reionization redshift of the instantaneous reionization model occurs at the midpoint of the inhomogeneous model.
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33

Ellewsen, Thor A. S., Bridget Falck, and David F. Mota. "Degeneracies between modified gravity and baryonic physics." Astronomy & Astrophysics 615 (July 2018): A134. http://dx.doi.org/10.1051/0004-6361/201731938.

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In order to determine the observable signatures of modified gravity theories, it is important to consider the effect of baryonic physics. We used a modified version of the ISIS code to run cosmological hydrodynamic simulations in order to study degeneracies between modified gravity and radiative hydrodynamic processes. One of the simulations was the standard Λ cold dark matter model and four were variations of the Symmetron model. For each model we ran three variations of baryonic processes: nonradiative hydrodynamics; cooling and star formation; and cooling, star formation, and supernova feedback. We constructed stacked gas density, temperature, and dark matter density profiles of the halos in the simulations, and studied the differences between them. We find that both radiative variations of the models show degeneracies between their processes and at least two of the three parameters defining the Symmetron model.
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34

Jappsen, Anne-Katharina, Simon C. O. Glover, Ralf S. Klessen, and Mordecai-Mark Mac Low. "Assessing the influence of metallicity on fragmentation of proto-galactic gas." Proceedings of the International Astronomical Union 2, no. 14 (August 2006): 268. http://dx.doi.org/10.1017/s1743921307010514.

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AbstractIn cold dark matter cosmological models, the first stars to form are believed to do so within small protogalaxies. We study the influence of low levels of metal enrichment on the cooling and collapse of ionized gas in these protogalactic halos using three-dimensional, smoothed particle hydrodynamics simulations.
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35

Frenk, C. S., S. D. M. White, P. Bode, J. R. Bond, G. L. Bryan, R. Cen, H. M. P. Couchman, et al. "The Santa Barbara Cluster Comparison Project: A Comparison of Cosmological Hydrodynamics Solutions." Astrophysical Journal 525, no. 2 (November 10, 1999): 554–82. http://dx.doi.org/10.1086/307908.

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36

Springel, V., and L. Hernquist. "Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation." Monthly Notices of the Royal Astronomical Society 339, no. 2 (February 21, 2003): 289–311. http://dx.doi.org/10.1046/j.1365-8711.2003.06206.x.

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37

Nagamine, K., V. Springel, and L. Hernquist. "Abundance of damped Lyman α absorbers in cosmological smoothed particle hydrodynamics simulations." Monthly Notices of the Royal Astronomical Society 348, no. 2 (February 2004): 421–34. http://dx.doi.org/10.1111/j.1365-2966.2004.07393.x.

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38

Steinmetz, Matthias. "Grapesph: cosmological smoothed particle hydrodynamics simulations with the special-purpose hardware GRAPE." Monthly Notices of the Royal Astronomical Society 278, no. 4 (February 1996): 1005–17. http://dx.doi.org/10.1093/mnras/278.4.1005.

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39

Zakharov, A. V., and I. V. Malanichev. "Transport coefficients and equations of hydrodynamics for the radiation-dominated cosmological plasma." Soviet Physics Journal 33, no. 5 (May 1990): 412–15. http://dx.doi.org/10.1007/bf00896079.

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40

Chan, T. K., Tom Theuns, Richard Bower, and Carlos Frenk. "Smoothed particle radiation hydrodynamics: two-moment method with local Eddington tensor closure." Monthly Notices of the Royal Astronomical Society 505, no. 4 (June 12, 2021): 5784–814. http://dx.doi.org/10.1093/mnras/stab1686.

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ABSTRACT We present a new smoothed particle hydrodynamics-radiative transfer method (sph-m1rt) that is coupled dynamically with sph. We implement it in the (task-based parallel) swift galaxy simulation code but it can be straightforwardly implemented in other sph codes. Our moment-based method simultaneously solves the radiation energy and flux equations in sph, making it adaptive in space and time. We modify the m1 closure relation to stabilize radiation fronts in the optically thin limit. We also introduce anisotropic artificial viscosity and high-order artificial diffusion schemes, which allow the code to handle radiation transport accurately in both the optically thin and optically thick regimes. Non-equilibrium thermochemistry is solved using a semi-implicit sub-cycling technique. The computational cost of our method is independent of the number of sources and can be lowered further by using the reduced speed-of-light approximation. We demonstrate the robustness of our method by applying it to a set of standard tests from the cosmological radiative transfer comparison project of Iliev et al. The sph-m1rt scheme is well-suited for modelling situations in which numerous sources emit ionizing radiation, such as cosmological simulations of galaxy formation or simulations of the interstellar medium.
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41

Simha, Vimal, David H. Weinberg, Romeel Davé, Oleg Y. Gnedin, Neal Katz, and Dušan Kereš. "The growth of central and satellite galaxies in cosmological smoothed particle hydrodynamics simulations." Monthly Notices of the Royal Astronomical Society 399, no. 2 (October 21, 2009): 650–62. http://dx.doi.org/10.1111/j.1365-2966.2009.15341.x.

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42

Nickerson, S., G. Stinson, H. M. P. Couchman, J. Bailin, and J. Wadsley. "Mechanisms of baryon loss for dark satellites in cosmological smoothed particle hydrodynamics simulations." Monthly Notices of the Royal Astronomical Society 415, no. 1 (May 9, 2011): 257–70. http://dx.doi.org/10.1111/j.1365-2966.2011.18700.x.

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43

Anbajagane, Dhayaa, August E. Evrard, Arya Farahi, David J. Barnes, Klaus Dolag, Ian G. McCarthy, Dylan Nelson, and Annalisa Pillepich. "Stellar property statistics of massive haloes from cosmological hydrodynamics simulations: common kernel shapes." Monthly Notices of the Royal Astronomical Society 495, no. 1 (April 28, 2020): 686–704. http://dx.doi.org/10.1093/mnras/staa1147.

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ABSTRACT We study stellar property statistics, including satellite galaxy occupation, of haloes in three cosmological hydrodynamics simulations: BAHAMAS + MACSIS, IllustrisTNG, and Magneticum Pathfinder. Applying localized linear regression, we extract halo mass-conditioned normalizations, slopes, and intrinsic covariance for (i) Nsat, the number of stellar mass-thresholded satellite galaxies within radius R200c of the halo; (ii) $M_{\star , \rm tot}$, the total stellar mass within that radius, and (iii) $M_{\star ,\rm BCG}$, the gravitationally bound stellar mass of the central galaxy within a $100 \, \rm kpc$ radius. The parameters show differences across the simulations, in part from numerical resolution, but there is qualitative agreement for the $N_{\rm sat}\!-\! M_{\star ,\rm BCG}$ correlation. Marginalizing over Mhalo, we find the Nsat kernel, $p(\ln N_{\rm sat}\, |\, M_{\rm halo}, z)$ to be consistently skewed left in all three simulations, with skewness parameter γ = −0.91 ± 0.02, while the $M_{\star , \rm tot}$ kernel shape is closer to lognormal. The highest resolution simulations find γ ≃ −0.8 for the z = 0 shape of the $M_{\star ,\rm BCG}$ kernel. We provide a Gaussian mixture fit to the low-redshift Nsat kernel as well as local linear regression parameters tabulated for $M_{\rm halo}\gt 10^{13.5} \, {\rm M}_\odot$ in all simulations.
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44

Night, C., K. Nagamine, V. Springel, and L. Hernquist. "Lyman break galaxies at z = 4–6 in cosmological smoothed particle hydrodynamics simulations." Monthly Notices of the Royal Astronomical Society 366, no. 3 (March 1, 2006): 705–16. http://dx.doi.org/10.1111/j.1365-2966.2005.09730.x.

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45

Hammami, A., and D. F. Mota. "Cosmological simulations with hydrodynamics of screened scalar-tensor gravity with non-universal coupling." Astronomy & Astrophysics 584 (November 20, 2015): A57. http://dx.doi.org/10.1051/0004-6361/201526606.

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46

Tissera, P. B., and D. G. Lambas. "Chemical Abundances and Hierarchical Clustering." Symposium - International Astronomical Union 217 (2004): 264–65. http://dx.doi.org/10.1017/s0074180900197682.

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In this contribution we study the chemical enrichment of the interstellar medium and stellar population of the building blocks of current typical galaxies in the field, in cosmological hydrodynamics simulations. The simulations include detailed modeling of chemical enrichment by SNIa and SNII In our simulations the missing metal problem is caused by chemical elements being locked up in stars, in the central regions (or bulges) mainly. Supernova energy feedback could help to reduce this concentration by expelling metals to the intergalactic medium.
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47

ROSU, H. C., and R. LÓPEZ-SANDOVAL. "BAROTROPIC FRW COSMOLOGIES WITH A DIRAC-LIKE PARAMETER." Modern Physics Letters A 19, no. 20 (June 28, 2004): 1529–35. http://dx.doi.org/10.1142/s0217732304013763.

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Using the known connection between Schrödinger-like equations and Dirac-like equations in the supersymmetric context, we discuss an extension of FRW barotropic cosmologies in which a Dirac mass-like parameter is introduced. New Hubble cosmological parameters HK(η) depending on the Dirac-like parameter are plotted and compared with the standard Hubble case H0(η). The new HK(η) are complex quantities. The imaginary part is a supersymmetric way of introducing dissipation and instabilities in the barotropic FRW hydrodynamics.
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48

Hennawi, Joe. "The Circumgalactic Medium of Quasars." Proceedings of the International Astronomical Union 9, S304 (October 2013): 355. http://dx.doi.org/10.1017/s174392131400430x.

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AbstractI will argue that observations of the diffuse gas in the outskirts of quasar host galaxies, or the so called circumgalactic medium, are essential for understanding how luminous quasars evolve in a cosmological context. Such observations also provide a fruitful comparison to theory, because hydrodynamics at moderate overdensities is much easier to simulate than the complicated processes which trigger quasar activity. A novel technique will be introduced, whereby a foreground quasar can be studied in absorption against a background quasar, resolving scales as small as 30 kpc. This experiment reveals a rich absorption spectrum which contains a wealth of information about the physical conditions of diffuse gas around quasars. Hydrodynamical simulations of the massive dark matter halos which host luminous quasars under predict the amount of cool gas observed in quasar environs by a large factor, challenging our understanding of how massive galaxies form. I will also discuss a very sensitive search for Ly-alpha emission from the same gas which we study in absorption.
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49

Ceverino, Daniel, and Anatoly Klypin. "The role of stellar feedback in the formation of galactic disks and bulges in a ΛCDM Universe." Proceedings of the International Astronomical Union 3, S245 (July 2007): 33–34. http://dx.doi.org/10.1017/s1743921308017213.

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AbstractAlthough supernova explosions and stellar winds happens at scales bellow 100 pc, they affect the interstellar medium (ISM) and galaxy formation. We use cosmological N-body+Hydrodynamics simulations of galaxy formation, as well as simulations of the ISM to study the effect of stellar feedback on galactic scales. Stellar feedback maintains gas with temperatures above a million degrees. This gas fills bubbles, super-bubbles and chimneys. Our model of feedback, in which 10%–30% of the feedback energy is coming from runaway stars, reproduces this hot gas only if the resolution is better than 50 pc. This is 10 times better than the typical resolution in cosmological simulations of galaxy formation. Only with this resolution, the effect of stellar feedback in galaxy formation is resolved without any assumption about sub-resolution physics. Stellar feedback can regulate the formation of bulges and can shape the inner parts of the rotation curve.
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50

Moriwaki, Kana. "The distribution and physical properties of high-redshift [Oiii] emitters in a cosmological hydrodynamics simulation." Proceedings of the International Astronomical Union 15, S341 (November 2019): 249–52. http://dx.doi.org/10.1017/s1743921319002424.

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AbstractAtacama Large Millimeter/submillimeter Array (ALMA) has enabled us to detect [Oiii] 88 μm line even at z > 9. To study the properties of high-redshift [Oiii] emitters, we calculate [Oiii] luminosities of galaxies in a cosmological simulation by applying a physical model of Hii region and using the photoionization code cloudy. We find that the [Oiii] 88 μm luminosity, LOIII,88, scales with SFR with slightly larger LOIII,88 than a local relation. Some [Oiii] emitters have extended disk-like structure. We propose to use the ratio between [Oiii] 88 μm line and [Oiii] 5007 Å line, which can be detected with James Webb Space Telescope (JWST), to estimate the gas density and the metallicity in HII region of high-redshift [Oiii] emitters.
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