<scp>SPLASH</scp>: An Interactive Visualisation Tool for Smoothed Particle Hydrodynamics Simulations

Price, Daniel J.

doi:10.1071/as07022

Cited by 699 publications

(448 citation statements)

References 20 publications

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“…Note that all values for secondary is divided by the initial mass ratio q 0 . All density maps in this paper are produced using SPLASH visualization code (Price 2007) that the mass ratio decreases, as ∆Mp and ∆Ms/q are compared here. In this case of q0 = 0.1, we see that the growth of ∆M b (t) is always dominated by that of the circum-primary disc M disc,p (t).…”

Section: Formation Of Discsmentioning

confidence: 99%

Evolution of binary seeds in collapsing protostellar gas clouds

Satsuka

Tsuribe

Tanaka

et al. 2016

Mon. Not. R. Astron. Soc.

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We perform three dimensional smoothed particle hydrodynamics (SPH) simulations of gas accretion onto the seeds of binary stars to investigate their short-term evolution. Taking into account of dynamically evolving envelope with non-uniform distribution of gas density and angular momentum of accreting flow, our initial condition includes a seed binary and a surrounding gas envelope, modelling the phase of core collapse of gas cloud when the fragmentation has already occurred. We run multiple simulations with different values of initial mass ratio q 0 (the ratio of secondary over primary mass) and gas temperature. For our simulation setup, we find a critical value of q c = 0.25 which distinguishes the later evolution of mass ratio q as a function of time. If q 0 q c , the secondary seed grows faster and q increases monotonically towards unity. If q 0 q c , on the other hand, the primary seed grows faster and q is lower than q 0 at the end of the simulation. Based on our numerical results, we analytically calculate the long-term evolution of the seed binary including the growth of binary by gas accretion. We find that the seed binary with q 0 q c evolves towards an equal-mass binary star, and that with q 0 q c evolves to a binary with an extreme value of q. Binary separation is a monotonically increasing function of time for any q 0 , suggesting that the binary growth by accretion does not lead to the formation of close binaries.

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Section: Formation Of Discsmentioning

confidence: 99%

Evolution of binary seeds in collapsing protostellar gas clouds

Satsuka

Tsuribe

Tanaka

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Bate et al 2010) and SMBH binaries accreting from the host galaxy (e.g. King & Pringle 2006, 2007King et al 2008). In both cases, a significant fraction of randomly oriented discs are expected to align or counteralign with the binary plane depending primarily on the initial disc-binary inclination angle, but also on the ratio of disc to binary angular momentum (King et al 2005;Nixon et al 2011b).…”

Section: Discussionmentioning

confidence: 99%

“…acknowledges support from NASA grant NNX11AK61G. We used splash (Price 2007) for the visualisation. This work utilised the Janus supercomputer, which is supported by the National Science Foundation (award number CNS-0821794) and the University of Colorado Boulder.…”

Section: Acknowledgmentsmentioning

confidence: 99%

Resonances in retrograde circumbinary discs

Nixon

Lubow

2015

Monthly Notices of the Royal Astronomical Society

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We analyse the interaction of an eccentric binary with a circular coplanar circumbinary disc that rotates in a retrograde sense with respect to the binary. In the circular binary case, no Lindblad resonances lie within the disc and no Lindblad resonant torques are produced, as was previously known. By analytic means, we show that when the binary orbit is eccentric, there exist components of the gravitational potential of the binary which rotate in a retrograde sense to the binary orbit and so rotate progradely with respect to this disc, allowing a resonant interaction to occur between the binary and the disc. The resulting resonant torques distinctly alter the disc response from the circular binary case. We describe results of three-dimensional hydrodynamic simulations to explore this effect and categorise the response of the disc in terms of modes whose strengths vary as a function of binary mass ratio and eccentricity. These mode strengths are weak compared to the largest mode strengths expected in the prograde case where the binary and disc rotate in the same sense. However, for sufficiently high binary eccentricity, resonant torques open a gap in a retrograde circumbinary disc, while permitting gas inflow on to the binary via gas streams. The inflow results in a time varying accretion rate on to the binary that is modulated over the binary orbital period, as was previously found to occur in the prograde case.

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“…We adopt the artificial viscosity prescription of Morris & Monaghan (1997) with the Balsara (1995) "switch", as described in Dunhill et al (2013), in order to minimise spurious numerical transport of angular momentum. We chose a version of the MM switch with both minimum and maximum α SPH for each particle (e.g., Price 2004), and set α min = 0.1 and α max = 2. We use the standard gadget-2 equation of state, so that pressure P i and density ρ i of particle i are related to its internal energy u i by the adiabatic index γ (which we take to be 5/3 throughout) via the form…”

Section: Simulationsmentioning

confidence: 99%

“…We also thank the anonymous referee for their comments which helped to clarify the paper. We used splash (Price 2007) This work used the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1.…”

Section: Acknowledgmentsmentioning

confidence: 99%

Misaligned accretion on to supermassive black hole binaries

Dunhill

Alexander

Nixon

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present the results of high-resolution numerical simulations of gas clouds falling onto binary supermassive black holes to form circumbinary accretion discs, with both prograde and retrograde cloud orbits. We explore a range of clouds masses and cooling rates. We find that for low mass discs that cool fast enough to fragment, prograde discs are significantly shorter-lived than similar discs orbiting retrograde with respect to the binary. For fragmenting discs of all masses, we also find that prograde discs fragment across a narrower radial region. If the cooling is slow enough that the disc enters a self-regulating gravitoturbulent regime, we find that alignment between the disc and binary planes occurs on a timescale primarily dictated by the disc thickness. We estimate realistic cooling times for such discs, and find that in the majority of cases we expect fragmentation to occur. The longer lifetime of lowmass fragmenting retrograde discs allows them to drive significant binary evolution, and may provide a mechanism for solving the 'last parsec problem'.

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SPLASH: An Interactive Visualisation Tool for Smoothed Particle Hydrodynamics Simulations

Cited by 699 publications

References 20 publications

Evolution of binary seeds in collapsing protostellar gas clouds

Evolution of binary seeds in collapsing protostellar gas clouds

Resonances in retrograde circumbinary discs

Misaligned accretion on to supermassive black hole binaries

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