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Verfasst von:Schaal, Kevin [VerfasserIn]   i
 Springel, Volker [VerfasserIn]   i
 Pakmor, Rüdiger [VerfasserIn]   i
 Pfrommer, Christoph [VerfasserIn]   i
Titel:Shock finding on a moving-mesh
Titelzusatz:II. Hydrodynamic shocks in the Illustris universe
Verf.angabe:Kevin Schaal, Volker Springel, Rüdiger Pakmor, Christoph Pfrommer, Dylan Nelson, Mark Vogelsberger, Shy Genel, Annalisa Pillepich, Debora Sijacki and Lars Hernquist
E-Jahr:2016
Jahr:04 July 2016
Umfang:25 S.
Fussnoten:Gesehen am 06.11.2017
Titel Quelle:Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
Ort Quelle:Oxford : Oxford Univ. Press, 1827
Jahr Quelle:2016
Band/Heft Quelle:461(2016), 4, Seite 4441-4465
ISSN Quelle:1365-2966
Abstract:Hydrodynamical 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 non-radiative 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 $$\mathcal {M}\approx 10$$ 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 radio-mode 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 1012 M⊙, 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.
DOI:doi:10.1093/mnras/stw1587
URL:Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.

kostenfrei: Volltext: http://dx.doi.org/10.1093/mnras/stw1587
 DOI: https://doi.org/10.1093/mnras/stw1587
Datenträger:Online-Ressource
Sprache:eng
K10plus-PPN:1565001567
Verknüpfungen:→ Zeitschrift

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