ORCID Profile
0000-0001-7689-0933
Current Organisations
Princeton University
,
Universitat Zurich
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Publisher: American Astronomical Society
Date: 24-12-2013
Publisher: Oxford University Press (OUP)
Date: 13-06-2011
Publisher: AIP
Date: 2010
DOI: 10.1063/1.3458467
Publisher: American Astronomical Society
Date: 22-07-2011
Publisher: EDP Sciences
Date: 03-03-2011
Publisher: Oxford University Press (OUP)
Date: 30-05-2022
Abstract: Turbulence in the interstellar medium (ISM) is crucial in the process of star formation. Shocks produced by supernova explosions, jets, radiation from massive stars, or galactic spiral-arm dynamics are amongst the most common drivers of turbulence in the ISM. However, it is not fully understood how shocks drive turbulence, in particular whether shock driving is a more solenoidal (rotational, ergence-free) or a more compressive (potential, curl-free) mode of driving turbulence. The mode of turbulence driving has profound consequences for star formation, with compressive driving producing three times larger density dispersion, and an order of magnitude higher star formation rate than solenoidal driving. Here, we use hydrodynamical simulations of a shock inducing turbulent motions in a structured, multiphase medium. This is done in the context of a laser-induced shock, propagating into a foam material, in preparation for an experiment to be performed at the National Ignition Facility (NIF). Specifically, we analyse the density and velocity distributions in the shocked turbulent medium, and measure the turbulence driving parameter $b=(\\sigma _{\\rho /\\langle \\rho \\rangle }^{2\\Gamma }-1)^{1/2}(1-\\sigma _{\\rho /\\langle \\rho \\rangle }^{-2})^{-1/2}\\mathcal {M}^{-1}\\Gamma ^{-1/2}$, with the density dispersion σρ/〈ρ〉, the turbulent Mach number $\\mathcal {M}$, and the polytropic exponent Γ. Purely solenoidal and purely compressive driving correspond to b ∼ 1/3 and b ∼ 1, respectively. Using simulations in which a shock is driven into a multiphase medium with structures of different sizes and Γ & 1, we find b ∼ 1 for all cases, showing that shock-driven turbulence is consistent with strongly compressive driving.
Publisher: Oxford University Press (OUP)
Date: 28-08-2014
Publisher: American Astronomical Society
Date: 22-12-2011
Publisher: Cambridge University Press (CUP)
Date: 06-2008
DOI: 10.1017/S1743921308027956
Abstract: To 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 s le of cosmological SPH disks, generated with GCD+ . These preliminary results are the first in our long-term Galactic Archaeology Simulation program.
Publisher: Oxford University Press (OUP)
Date: 22-05-2012
Publisher: American Physical Society (APS)
Date: 21-06-2022
No related grants have been discovered for Romain Teyssier.