ORCID Profile
0000-0002-2137-4146
Current Organisation
University of Leeds
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Publisher: Oxford University Press (OUP)
Date: 25-07-2018
Publisher: Oxford University Press (OUP)
Date: 28-03-2012
Publisher: American Astronomical Society
Date: 21-07-2014
Publisher: Cambridge University Press (CUP)
Date: 2018
DOI: 10.1017/PASA.2018.25
Abstract: We present Phantom , a fast, parallel, modular, and low-memory smoothed particle hydrodynamics and magnetohydrodynamics code developed over the last decade for astrophysical applications in three dimensions. The code has been developed with a focus on stellar, galactic, planetary, and high energy astrophysics, and has already been used widely for studies of accretion discs and turbulence, from the birth of planets to how black holes accrete. Here we describe and test the core algorithms as well as modules for magnetohydrodynamics, self-gravity, sink particles, dust–gas mixtures, H 2 chemistry, physical viscosity, external forces including numerous galactic potentials, Lense–Thirring precession, Poynting–Robertson drag, and stochastic turbulent driving. Phantom is hereby made publicly available.
Publisher: Oxford University Press (OUP)
Date: 02-09-2019
Abstract: We investigate the impact of time-resolved ‘gradual’ stellar feedback processes in high redshift dwarf spheroidal galaxies. Here ‘gradual’ feedback refers to in idual stellar feedback events which deposit energy over a period of time. We conduct high-resolution hydrodynamical simulations of dwarf spheroidal galaxies with halo masses of 107–108 M⊙, based on z = 6 progenitors of the Milky Way’s dwarf spheroidal galaxies. We also include a novel feedback prescription for in idual massive stars, which includes stellar winds and an HMXB (high mass X-ray binary) phase, on top of supernovae. We find the mass of gas unbound across a 1 Gyr starburst is uniformly lowered if gradual feedback mechanisms are included across the range of metallicities, halo concentration parameters, and galaxy masses studied here. Furthermore, we find including gradual feedback in the smallest galaxies delays the unbinding of the majority of the gas and facilitates the production of ‘chimneys’ in the dense shell surrounding the feedback generated hot, pressurized ‘superbubble’. These ‘chimneys’ vent hot gas from the galaxy interior, lowering the temperature of the central 10 kpc of the gaseous halo. Additionally, we find radiative cooling has little effect on the energetics of simulations that include a short, violent starburst compared with those that have a longer, less concentrated starburst. Finally, we investigate the relative impact of HMXB feedback and stellar winds on our results, finding the ubiquity of stellar winds throughout each starburst makes them a defining factor in the final state of the interstellar medium.
Publisher: Oxford University Press (OUP)
Date: 30-07-2013
Publisher: American Astronomical Society
Date: 11-09-2012
Publisher: Oxford University Press (OUP)
Date: 12-2015
Publisher: Oxford University Press (OUP)
Date: 13-02-2015
DOI: 10.1093/MNRAS/STV014
Publisher: Oxford University Press (OUP)
Date: 30-10-2015
Publisher: American Astronomical Society
Date: 26-08-2014
Publisher: Oxford University Press (OUP)
Date: 23-03-2015
DOI: 10.1093/MNRAS/STV347
Location: United Kingdom of Great Britain and Northern Ireland
Location: United Kingdom of Great Britain and Northern Ireland
Location: United Kingdom of Great Britain and Northern Ireland
No related grants have been discovered for Christopher Nixon.