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Hydrodynamical Adaptive Mesh Refinement Simulations of Disk Galaxies

Published online by Cambridge University Press:  01 June 2008

Brad K. Gibson ,
Stéphanie Courty ,
Patricia Sánchez-Blázquez ,
Romain Teyssier ,
Elisa L. House ,
Chris B. Brook  and
Daisuke Kawata
Brad K. Gibson
Affiliation:
Centre for Astrophysics, University of Central Lancashire, Preston, PR1 2HE, UK email: [email protected]
Stéphanie Courty
Affiliation:
Centre for Astrophysics, University of Central Lancashire, Preston, PR1 2HE, UK email: [email protected]
Patricia Sánchez-Blázquez
Affiliation:
Centre for Astrophysics, University of Central Lancashire, Preston, PR1 2HE, UK email: [email protected]
Romain Teyssier
Affiliation:
Service d'Astrophysique, CEA Saclay, Batiment 709, 91191 Gif sur Yvette, France
Elisa L. House
Affiliation:
Centre for Astrophysics, University of Central Lancashire, Preston, PR1 2HE, UK email: [email protected]
Chris B. Brook
Affiliation:
Centre for Astrophysics, University of Central Lancashire, Preston, PR1 2HE, UK email: [email protected]
Daisuke Kawata
Affiliation:
Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA, 91101, USA
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Abstract

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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 sample of cosmological SPH disks, generated with GCD+. These preliminary results are the first in our long-term Galactic Archaeology Simulation program.

Keywords

galaxies: formationgalaxies: evolutionmethods: n-body simulations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S254: The Galaxy Disk in Cosmological Context , June 2008 , pp. 445 - 452
Copyright
Copyright © International Astronomical Union 2009

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