SEREN – a new SPH code for star and planet formation simulations

Hubber, D. A.; Batty, Christopher; McLeod, Andrew; Whitworth, Anthony Peter

doi:10.1051/0004-6361/201014949

Cited by 100 publications

(111 citation statements)

References 73 publications

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“…We use an MPI-parallelized version of the SEREN (Hubber et al, 2010) code to simulate cloud-cloud collisions with smoothed particle hydrodynamics (SPH). We include self-gravity.…”

Section: Methodsmentioning

confidence: 99%

Collisions of supersonic clouds

McLeod

Palouš

Whitworth³

2010

Proc. IAU

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Abstract. We present simulations of supersonic collisions between molecular clouds of mass 500 M and radius 2.24 pc. The simulations are performed with the SEREN SPH code. The code treats the energy equation and the associated transport of heating and cooling radiation. The formation of protostars is captured by introducing sink particles. Low velocity collisions form a shock-compressed layer which fragments to form stars. For high-velocity collisions, v r el 5 km s −1 , the non-linear thin shell instability strongly disrupts the shock-compressed layer, and may inhibit the formation of stars.

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“…We use an MPI-parallelized version of the SEREN (Hubber et al, 2010) code to simulate cloud-cloud collisions with smoothed particle hydrodynamics (SPH). We include self-gravity.…”

Section: Methodsmentioning

confidence: 99%

Collisions of supersonic clouds

McLeod

Palouš

Whitworth³

2010

Proc. IAU

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“…Numerical simulations were performed using the well-tested smoothed particle hydrodynamics (SPH) code SEREN in its energy and momentum conserving formalism with an adaptive gravitational softening length (Hubber et al 2011). Simulations were developed with the standard cubic spline kernel with each SPH particle having approximately 50 neighbours.…”

Section: Numerical Algorithmmentioning

confidence: 99%

Formation of Prestellar Cores via Non-Isothermal Gas Fragmentation

Anathpindika

2015

Publ. Astron. Soc. Aust.

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Sheet-like clouds are common in turbulent gas and perhaps form via collisions between turbulent gas flows. Having examined the evolution of an isothermal shocked slab in an earlier contribution, in this work we follow the evolution of a sheet-like cloud confined by (thermal) pressure and gas in it is allowed to cool. The extant purpose of this endeavour is to study the early phases of core-formation. The observed evolution of this cloud supports the conjecture that molecular clouds themselves are three-phase media (comprising viz. a stable cold and warm medium, and a third thermally unstable medium), though it appears, clouds may evolve in this manner irrespective of whether they are gravitationally bound. We report, this sheet fragments initially due to the growth of the thermal instability (TI) and some fragments are elongated, filament-like. Subsequently, relatively large fragments become gravitationally unstable and sub-fragment into smaller cores. The formation of cores appears to be a three stage process: first, growth of the TI leads to rapid fragmentation of the slab; second, relatively small fragments acquire mass via gas-accretion and/or merger and third, sufficiently massive fragments become susceptible to the gravitational instability and sub-fragment to form smaller cores. We investigate typical properties of clumps (and smaller cores) resulting from this fragmentation process. Findings of this work support the suggestion that the weak velocity field usually observed in dense clumps and smaller cores is likely seeded by the growth of dynamic instabilities. Simulations were performed using the smooth particle hydrodynamics algorithm.

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“…The implementation strategy, however, is not restricted to this type of tree and can straightforwardly be adapted to other tree types such as octree (Barnes & Hut 1986) or other binary trees (Benz et al 1990). The RCB tree is not built down to the last particle, but down to small groups of adjacent particles that are always aggregated into what we call "lowest-level cells" (or ll-cells), also found in the "tree literature" as "leaves" (Oxley & Woolfson 2003;Springel 2005;Gaburov et al 2010;Hubber et al 2011;Clark et al 2012) or as "buckets" (Dikaiakos & Stadel 1996;Stadel 2001;Wadsley et al 2004). Since the average number of particles per ll-cell (typically ∼12) is much smaller than the average neighbor number (∼100), the size of any ll-cell will always be smaller than the smoothing length of its particles.…”

Section: Performing the Integrationmentioning

confidence: 99%

MODA: a new algorithm to compute optical depths in multidimensional hydrodynamic simulations

Perego

Gafton

Cabezón

et al. 2014

A&A

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Aims. We introduce the multidimensional optical depth algorithm (MODA) for the calculation of optical depths in approximate multidimensional radiative transport schemes, equally applicable to neutrinos and photons. Motivated by (but not limited to) neutrino transport in three-dimensional simulations of core-collapse supernovae and neutron star mergers, our method makes no assumptions about the geometry of the matter distribution, apart from expecting optically transparent boundaries. Methods. Based on local information about opacities, the algorithm figures out an escape route that tends to minimize the optical depth without assuming any predefined paths for radiation. Its adaptivity makes it suitable for a variety of astrophysical settings with complicated geometry (e.g., core-collapse supernovae, compact binary mergers, tidal disruptions, star formation, etc.). We implement the MODA algorithm into both a Eulerian hydrodynamics code with a fixed, uniform grid and into an SPH code where we use a tree structure that is otherwise used for searching neighbors and calculating gravity. Results. In a series of numerical experiments, we compare the MODA results with analytically known solutions. We also use snapshots from actual 3D simulations and compare the results of MODA with those obtained with other methods, such as the global and local ray-by-ray method. It turns out that MODA achieves excellent accuracy at a moderate computational cost. In appendix we also discuss implementation details and parallelization strategies.

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SEREN – a new SPH code for star and planet formation simulations

Cited by 100 publications

References 73 publications

Collisions of supersonic clouds

Collisions of supersonic clouds

Formation of Prestellar Cores via Non-Isothermal Gas Fragmentation

MODA: a new algorithm to compute optical depths in multidimensional hydrodynamic simulations

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