| Online-Ressource |
Verfasst von: | Schaal, Kevin [VerfasserIn]  |
| Springel, Volker [VerfasserIn]  |
| Pakmor, Rüdiger [VerfasserIn]  |
| Pfrommer, Christoph [VerfasserIn]  |
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 |
Shock finding on a moving-mesh / Schaal, Kevin [VerfasserIn]; 04 July 2016 (Online-Ressource)