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dc.contributor.authorSchaal, Ken
dc.contributor.authorSpringel, Ven
dc.contributor.authorPakmor, Ren
dc.contributor.authorPfrommer, Cen
dc.contributor.authorNelson, Den
dc.contributor.authorVogelsberger, Men
dc.contributor.authorGenel, Sen
dc.contributor.authorPillepich, Aen
dc.contributor.authorSijacki, Deboraen
dc.contributor.authorHernquist, Len
dc.date.accessioned2017-05-31T14:42:58Z
dc.date.available2017-05-31T14:42:58Z
dc.date.issued2016-10-01en
dc.identifier.issn0035-8711
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/264548
dc.description.abstractHydrodynamical shocks are a manifestation of the non-linearity of the Euler equations and play a fundamental role in cosmological gas dynamics. In this work, we identify and analyse shocks in the Illustris simulation, and contrast the results with those of non-radiative runs.We show that simulations with more comprehensive physical models of galaxy formation pose new challenges for shock finding algorithms due to radiative cooling and star-forming processes,prompting us to develop a number of methodology improvements. We find in Illustris a total shock surface area which is about 1.4 times larger at the present epoch compared to nonradiative runs, and an energy dissipation rate at shocks which is higher by a factor of around 7.Remarkably, shocks with Mach numbers above and below M ≈ 10 contribute about equally to the total dissipation across cosmic time. This is in sharp contrast to non-radiative simulations,and we demonstrate that a large part of the difference arises due to strong black hole radiomode feedback in Illustris. We also provide an overview of the large diversity of shock morphologies, which includes complex networks of halo-internal shocks, shocks on to cosmic sheets, feedback shocks due to black holes and galactic winds, as well as ubiquitous accretion shocks. In high-redshift systems more massive than 1012M⊙, we discover the existence of a double accretion shock pattern in haloes. They are created when gas streams along filaments without being shocked at the outer accretion shock, but then forms a second, roughly spherical accretion shock further inside.
dc.description.sponsorshipKS and VS acknowledge support through subproject EXAMAG of the Priority Programme 1648 SPPEXA of the German Science Foundation, and the European Research Council through ERC-StG grant EXAGAL-308037. CP acknowledges support through the ERC-CoG grant CRAGSMAN-646955. SG acknowledges support provided by NASA through Hubble Fellowship grant HST-HF2-51341.001-A awarded by the STScI, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. DS acknowledges support by the STFC and the ERC Starting Grant 638707 ‘BHs and their host galaxies: co-evolution across cosmic time’. LH acknowledges support from NASA grant NNX12AC67G and NSF grant AST-1312095. KS, VS, RP, and CP like to thank the Klaus Tschira Foundation, and KS acknowledges support by the IMPRS for Astronomy and Cosmic Physics at the University of Heidelberg.
dc.language.isoenen
dc.publisherOxford University Press
dc.subjecthydrodynamicsen
dc.subjectshock wavesen
dc.subjectmethods: numericalen
dc.subjectgalaxies: clusters: generalen
dc.subjectgalaxies: kinematics and dynamicsen
dc.subjectlarge-scale structure of Universeen
dc.titleShock finding on a moving-mesh - II. Hydrodynamic shocks in the Illustris universeen
dc.typeArticle
prism.endingPage4465
prism.issueIdentifier4en
prism.publicationDate2016en
prism.publicationNameMonthly Notices of the Royal Astronomical Societyen
prism.startingPage4441
prism.volume461en
dc.identifier.doi10.17863/CAM.10116
dcterms.dateAccepted2016-06-30en
rioxxterms.versionofrecord10.1093/mnras/stw1587en
rioxxterms.versionVoRen
rioxxterms.licenseref.urihttp://www.rioxx.net/licenses/all-rights-reserveden
rioxxterms.licenseref.startdate2016-10-01en
dc.contributor.orcidSijacki, Debora [0000-0002-3459-0438]
dc.identifier.eissn1365-2966
rioxxterms.typeJournal Article/Reviewen
pubs.funder-project-idECH2020 EUROPEAN RESEARCH COUNCIL (ERC) (638707)
cam.issuedOnline2016-07-04en


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