A general class of Lagrangian smoothed particle hydrodynamics methods and implications for fluid mixing problems

Various formulations of smooth-particle hydrodynamics (SPH) have been proposed, intended to resolve certain difficulties in the treatment of fluid mixing instabilities. Most have involved changes to the algorithm which either introduce artificial correction terms or violate arguably the greatest advantage of SPH over other methods: manifest conservation of energy, entropy, momentum, and angular momentum. Here, we show how a class of alternative SPH equations of motion (EOM) can be derived self-consistently from a discrete particle Lagrangian (guaranteeing manifest conservation) in a manner which tremendously improves treatment of instabilities and contact discontinuities. Saitoh & Makino recently noted that the volume element used to discretize the EOM does not need to explicitly invoke the mass density (as in the 'standard' approach); we show how this insight, and the resulting degree of freedom, can be incorporated into the rigorous Lagrangian formulation that retains ideal conservation properties and includes the 'Grad-h' terms that account for variable smoothing lengths. We derive a general EOM for any choice of volume element (particle 'weights') and method of determining smoothing lengths. We then specify this to a 'pressure-entropy formulation' which resolves problems in the traditional treatment of fluid interfaces. Implementing this in a new version of the GADGET code, we show it leads to good performance in mixing experiments (e.g. Kelvin-Helmholtz & blob tests). And conservation is maintained even in strong shock/blastwave tests, where formulations without manifest conservation produce large errors. This also improves the treatment of sub-sonic turbulence, and lessens the need for large kernel particle numbers. The code changes are trivial and entail no additional numerical expense. This provides a general framework for self-consistent derivation of different 'flavors' of SPH.

[1]  Daniel J. Price Modelling discontinuities and Kelvin-Helmholtz instabilities in SPH , 2007, J. Comput. Phys..

[2]  Peter A. Thomas,et al.  Multiphase smoothed-particle hydrodynamics , 2001 .

[3]  V. Springel Smoothed Particle Hydrodynamics in Astrophysics , 2010, 1109.2219.

[4]  Stephan Rosswog,et al.  Conservative, special-relativistic smoothed particle hydrodynamics , 2009, J. Comput. Phys..

[5]  J. Monaghan,et al.  Smoothed particle hydrodynamics: Theory and application to non-spherical stars , 1977 .

[6]  J. Monaghan,et al.  A Switch to Reduce SPH Viscosity , 1997 .

[7]  Garching,et al.  Smoothed particle hydrodynamics for galaxy‐formation simulations: improved treatments of multiphase gas, of star formation and of supernovae feedback , 2003 .

[8]  L. Lucy A numerical approach to the testing of the fission hypothesis. , 1977 .

[9]  O. Agertz,et al.  Resolving mixing in smoothed particle hydrodynamics , 2009, 0906.0774.

[10]  Daniel J. Price,et al.  Algorithmic comparisons of decaying, isothermal, supersonic turbulence , 2008, 0810.4599.

[11]  Volker Springel,et al.  Moving‐mesh cosmology: characteristics of galaxies and haloes , 2011, 1109.4638.

[12]  U. Berkeley,et al.  Moving mesh cosmology: the hydrodynamics of galaxy formation , 2011, 1109.3468.

[13]  V. Springel,et al.  Moving-mesh cosmology: properties of gas discs , 2011, 1110.5635.

[14]  J. Monaghan,et al.  Fundamental differences between SPH and grid methods , 2006, astro-ph/0610051.

[15]  Ding Xin,et al.  On criterions for smoothed particle hydrodynamics kernels in stable field , 2005 .

[16]  Walter Dehnen,et al.  Inviscid smoothed particle hydrodynamics , 2010 .

[17]  C. D. Vecchia,et al.  Implementation of feedback in SPH: towards concordance of methods , 2011, 1105.3729.

[18]  P. Hopkins,et al.  The structure of the interstellar medium of star‐forming galaxies , 2011, 1110.4636.

[19]  V. Springel E pur si muove: Galilean-invariant cosmological hydrodynamical simulations on a moving mesh , 2009, 0901.4107.

[20]  Dennis W. Quinn,et al.  An Analysis of 1-D Smoothed Particle Hydrodynamics Kernels , 1996 .

[21]  Daniel J. Price,et al.  A comparison between grid and particle methods on the statistics of driven, supersonic, isothermal turbulence , 2010, 1004.1446.

[22]  Volker Springel,et al.  Cosmological SPH simulations: The entropy equation , 2001 .

[23]  James Wadsley,et al.  On the treatment of entropy mixing in numerical cosmology , 2008 .

[24]  G. Dilts MOVING-LEAST-SQUARES-PARTICLE HYDRODYNAMICS-I. CONSISTENCY AND STABILITY , 1999 .

[25]  Harvard,et al.  Stellar feedback and bulge formation in clumpy discs , 2011, 1111.6591.

[26]  Junichiro Makino,et al.  A DENSITY-INDEPENDENT FORMULATION OF SMOOTHED PARTICLE HYDRODYNAMICS , 2012, 1202.4277.

[27]  G. Snyder,et al.  The Magnetohydrodynamics of Shock-Cloud Interaction in Three Dimensions , 2008, 0802.2708.

[28]  J. Read,et al.  SPHS: Smoothed Particle Hydrodynamics with a higher order dissipation switch , 2011, 1111.6985.

[29]  Volker Springel,et al.  Moving mesh cosmology: numerical techniques and global statistics , 2011, 1109.1281.

[30]  J. Makino,et al.  A NECESSARY CONDITION FOR INDIVIDUAL TIME STEPS IN SPH SIMULATIONS , 2008, 0808.0773.

[31]  Tom Abel,et al.  rpSPH: a novel smoothed particle hydrodynamics algorithm , 2010, 1003.0937.

[32]  W. Dehnen,et al.  Improving convergence in smoothed particle hydrodynamics simulations without pairing instability , 2012, 1204.2471.

[33]  Momentum transfer across shear flows in smoothed particle hydrodynamic simulations of galaxy formation , 2003, astro-ph/0306568.

[34]  A. Frank,et al.  The Magnetohydrodynamic Kelvin-Helmholtz Instability: A Two-dimensional Numerical Study , 1995, astro-ph/9510115.

[35]  Joseph P. Morris,et al.  A Study of the Stability Properties of Smooth Particle Hydrodynamics , 1996, Publications of the Astronomical Society of Australia.

[36]  Volker Springel,et al.  Particle hydrodynamics with tessellation techniques , 2009, 0912.0629.

[37]  Stephan Rosswog,et al.  Astrophysical smooth particle hydrodynamics , 2009, 0903.5075.

[38]  P. Hopkins,et al.  Stellar Feedback in Galaxies and the Origin of Galaxy-scale Winds , 2011, 1110.4638.

[39]  Andreas Bauer,et al.  Shocking results without shocks: Subsonic turbulence in smoothed particle hydrodynamics and moving-mesh simulations , 2011, 1109.4413.

[40]  Daniel J. Price Smoothed particle hydrodynamics and magnetohydrodynamics , 2010, J. Comput. Phys..

[41]  V. Springel,et al.  Cosmological smoothed particle hydrodynamics simulations: the entropy equation , 2001, astro-ph/0111016.

[42]  J. Monaghan,et al.  Implicit SPH Drag and Dusty Gas Dynamics , 1997 .

[43]  P. Hopkins,et al.  Self-regulated star formation in galaxies via momentum input from massive stars , 2011, 1101.4940.

[44]  Sergei Nayakshin,et al.  Kelvin-Helmholtz instabilities with Godunov smoothed particle hydrodynamics , 2010 .

[45]  Riccardo Brunino,et al.  Hydrodynamic simulations with the Godunov SPH , 2011, 1105.1344.

[46]  Joseph John Monaghan,et al.  On the fragmentation of differentially rotating clouds , 1983 .

[47]  M. Norman,et al.  Shock interactions with magnetized interstellar clouds. 1: Steady shocks hitting nonradiative clouds , 1994 .

[48]  I. J. Schoenberg Contributions to the problem of approximation of equidistant data by analytic functions. Part A. On the problem of smoothing or graduation. A first class of analytic approximation formulae , 1946 .

[49]  C. D. Vecchia,et al.  Implementation of feedback in smoothed particle hydrodynamics: towards concordance of methods , 2012 .