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Structures Formation in Extragalactic Astrophysics and
Cosmology: numerical approaches
G. Murante
SAIT, Pisa, May 7th
WhyWhy
Non linear evolution of Dark Matter density fluctuations (gravitational instability): no general analitic solution
..adding baryons: hydrodynamics required, even worse
Subgrid astrophysical processes (radiative cooling, star formation, Sne energy feedback, AGN feedback…): not even understood in full details
WhereWhere
Cosmology: LSSCosmology: high redshift structures (Damped Ly, high Z galaxies, protoclusters..)Galaxy cluster formation, evolution, properties; AGN/cluster connectionEarly type galaxy formation and evolution; DSCDisk galaxy formation
HowHow
N-Body (particle) codes for following gravitational instability from CMB on..Vlasov-Poisson (Boltzsmann) equationsHydro codes for the gas evolutionEuler equationsSubgrid parametric models for a number of astrophysical processesHPC required!
N-Body codesN-Body codes
A density field is sampled with massive particles
Gravitational forces evaluated in a newtonian way
General relativity enters in the background evolution ( cosmological model a(t) )
N-Body N-Body methodsmethods
Direct summationParticle-MeshParticle-Particle/Particle-MeshTree Codes
Adaptive P3M, Tree-PM…..
F i
Gm2(x i
x j )
2 x i
x j
2 3 / 2j
Hydrodynamical methodsHydrodynamical methods
Eulerian (grid-based) methods: evolution of hydrodynamical quantities at fixed spatial (grid) position, by directly solving the Euler equation.
Disadvantage: limited resolution (overcome with AMR codes)
Advantage: Euler equation directly solved
Lagrangian methods (SPH): hydrodynamical quantities attached to gas particles; evolution followed along the particle orbits; hydro forces exchanged along with gravitational forces
Disadvantage: it’s a mimic to true hydrodynamics
Advantage: high resolution achievable thanks to Lagrangian treatment (not bounded to the mesh size).
Other (astro)physical processesOther (astro)physical processes
Star formation/feedback – subgrid, but: bruteforceChemical enrichment / SNIa - subgridMetal/Atomic/Molecular cooling - exactMagnetic field – exact (simpler cases)BH/AGN feedback - subgridCosmic rays - subgridThermal conduction - exactNavier-Stokes - exactRadiative transport – approximate!…..
Available codesAvailable codes
GADGET (Springel 2001, 2005)
HYDRA (Couchman & Pearce 1995)
FLASH (Fryxell et al 2000)
ENZO (O’Shea et al 2004)
GASOLINE (Wadsley, Stadel, Quinn 2004)
RAMSES (Teyssier, 2002)
ART (Klypin, 1997; Kravtsov 1999)
…and many others…
Code validationCode validationStandard gravity/hydro tests
Code comparison (e.g. Santa Barbara Cluster Comparison, Frenk et al, 1999, ApJ, 525, 554)
Eulerian
Lagrangian
Open questionsOpen questions
GRAVITY: ok, except softening/resolution (BUT: full GR treatment, probably not needed; modified gravities..) …60 order of magnitude in mass approx… Boltzsmann
codes??
SPH: artificial viscosity; turbulence not well resolvedEULERIAN: not Galilean invariant? Numerical viscosity/mixing not well controlled..and of course, SUBGRID processes…
Mixed schemes: AREPO Mixed schemes: AREPO (Springel 2009)(Springel 2009)
Voronoi tassellation, centeredon gas particles
Mixed schemes: AREPO Mixed schemes: AREPO (Springel 2009)(Springel 2009)
Fluxes evaluated through thecell interfaces, resolvingthe corresponding Riemann problems
KH instability: comparison between AREPOand an Eulerian code (ATHENA)Note: SPH would perform miserably here
Mixed schemes: GPHMixed schemes: GPH
Riemann problem solved between all particle couplesP*, v* found and put in SPH equations (can be derived..)Artificial viscosity dropped
Imaeda & Inutsuka 2002Inutsuka 1994, 2002Inutsuka & Imaeda 2001Cha 2002Cha & Withworth 2003
Fluid mixing!
GPH in GADGET: SOD tube test (Murante, Borgani, Brunino, ..in prep?)
“blip” “whiggles”No whiggles!Blip reduced!mixing
Star formation, feedback…Star formation, feedback…simpler schemessimpler schemes
Dark Matter
Gas
StarsStar formation
Gravity only
Gravity + hydrodynamics
Density/temperaturethreshold
UV heat.
SN
RadiativeCooling
Kinetic FB
Star formation, feedback…Star formation, feedback…MultiPhase schemesMultiPhase schemes
Dark Matter
Hot gas
Cold gas
Stars
RadiativeCooling
StarFormationGravity
SN
UV heat.
Gravity only
Gravity + Hydro
MOLECULAR GASMOLECULAR GAS
cMcM
M
M
hM
hM
=
= =
MUPPIMUPPIMurante,
Monaco,
Giovalli,
Borgani,
Diaferio
sfM
sfM
STAR
FO
RM
ATIO
Ndyn
Hstarsf t
f MM 2
restM
RESTORATION
restM
sfrestrest MM f
coolM
coolM
CO
OLIN
G
cool
hcool t
MM
EVAPO
RATIO
N
evapM
evapM
dyn
Hevapevap t
f MM 2
MH2 ->SF
On hotphase!
On coldphase!