PLUTO: a modular code for computational astrophysics

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PLUTOa modular code for computational
astrophysics

• Developers A. Mignone1,2, G. Bodo2
• 1 The University of Chicago, ASC FLASH Center
• 2 INAF Osseratorio Astronomico di Torino
• 3 Universita degli studi di Torino
• 4 Universita degli studi di Firenze

C. Zanni3, T. Laverne2 , F. Rubini4, S.
Massaglia3, A. Rogava3, A. Ferrari3
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OUTLINE

• Written in C ( 33,000 lines)
• Explicit, compressible code (FV)
• Shock capturing
• High-mach number flows
• Works in 1, 2, 3-D
• Modular structure
• Physics
• Time stepping
• Interpolations
• Riemann Solvers
• No AMR
• Geometry support (Cart, Cyl, Spher)
• Serial/Parallel Implementation (MPI)

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Requirements

• (ANSI) C compiler
• Python (v. gt 1.6)
• GNU Make

Optional

• MPI (arraylib by A. Malagoli)
• GD graphics library

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PLUTO Fundamentals
PHYSICS Modules
TIME_STEPPING
Geometry\ Grid Generation
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Source Tree
Update
Un
Un1
Sources
Interpolation
physics modules
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Hydrodynamics (HD) Module
Eos
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Relativistic Hydrodynamics (RHD) Module

• Multi dimensional PPM, full corner coupled
  transport (Colella 1990)
• Nonlinear Riemann solver w/ general Eos (Mignone
  et al. submitted to ApJ), ? FLASH Code

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Magnetohydrodynamics (MHD) Module

• Monopole Control
• Powell (Powell 94)
• Monopole Diffusion (Marder 87)
• Flux CT (Balsara 2004)
• Splitting of Magnetic Field, B B0(x) B1(x,t)
  suitable for low-? plasma.

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Relativistic Magnetohydrodynamics (RMHD) Module

• Shares Features w/ MHD and RHD

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Algorithms

Time Stepping
HD RHD MHD RMHD

• Fwd Euler (Split/Unsplit)
• RK 2nd (Split/Unsplit)
• RK 3rd (Split/Unsplit)
• Hancock (Split/CTU)
• Characteristic Tracing (Split/CTU)

? ? ? ? ?
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? ? ? ? ?(split)
? ? ? ?(split) ?

Riemann Solvers

• Riemann (non-linear)
• TVD/ROE
• HLL
• TVDLF

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Interpolation

• Prim. TVD-limited (II order)
• Characteristic TVD-limited
• Piecewise-Parabolic
• Multi-D Linear Interpolation
• 2nd and 3rd order WENO

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Additional Features

• Particles (T. Laverne)
• Optically thin radiative losses
• power-law ?2T? ? (Analytic integrator)
• Interstellar cooling function
• T gt 104 K, Dalgarno McCray Cooling (1972)
• T lt 104 K, NEQ (H H2) (Oliva, 1992)
• NEQ cooling function for shocks lt 80 Km/s
• (Raymond 1987)
• Implicit Thermal Conduction (1-D only)

Explicit /Implicit 2nd order integrators
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Problem Setup

• Python Interface
• definitions.h
• makefile
• User
• 3. init.c
• Set initial conditions
• userdef b. c.
• Bckgr. B
• Gravity
• 4. pluto.ini
• CFL
• Domain
• output freq.

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Test Gallery
2-D Riemann Problem (HD)
2-D Riemann Problem (RHD)
Shock-Cloud Interaction(MHD)
RMHD Blast Wave
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Applications
Axisymmetric MHD Jet Mach 50 ? 1 ?in/?out
1/20
Keplerian Disk (Murante et al. 2004) Vortex-wave
generation
3D RHD Jet (Rossi et at. 2003) Mach3 ?
10 ?in/?out 1.e-4
2D RHD KH V 0.95c M 1.17
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More Applications
Thermally unstable radiative shocks (Mignone,
submitted to ApJ)
Accretion Column onto white dwarf
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Summary

• Simple, fast code for single/multi proc.
• User-friendly
• versatile
• suitable for algorithm comparison
• (fairly) well documented

gtgt Official release Feb 2005 ltlt
mignone_at_oddjob.uchicago.edu, bodo_at_to.astro.it