The Astrophysical MUltiscale
Software Environment (AMUSE)
P
-
I: Portegies Zwart
Co
-
Is: Nelemans, Pols, O’Nuallain, Spaans
Adv.: Langer, Tolstoy, Hut, Ercolano, de Grijs,
Mellema, Spurzem, Bischof, Quillen
AMUSE
The objectives of AMUSE
More science with existing software
Combine existing astrophysical codes
This is a technical problem
It is technically possible
Impression of how it works
Existing codes
Excellent single
-
physics codes exist
hydro
gravity
radiation
stellar evolution
All written in different languages, different
format, different architecture....
Need a homogeneous environment for utilizing
these resources
More science with existing code
Universe is multi
-
physics ...
Scientific objectives:
dense stellar systems (hydro+gravity+stellar evo.)
evolution of galactic environments, star formation,
AGN, ... (hydro+gravity+radiation)
planet formation (hydro+gravity+radiation)
galaxy formation and interaction
(gravity+hydro+radiation+stellar evo.)
Single physics software solutions exist, try to
combine existing codes
This is a technical problem
No new physics needed
Combining requires understanding of how
software and computer hardware interacts
Development to a usefull toolbox requires
professional engineering
Requires substantial manpower
It is technically feasible
Developing new code not optimal because
it is a time consuming task
large codes tend to become unmanageable
initial assumptions tend to require redesign at a late
stage in the development process
Combining existing code via wrapper has been
tried, and works
Propose homogeneous software framework,
à
la Numerical Recipes
Flow control layer (scripting language)
Gas dynamics
Radiative
transport
Stellar evolution
Stellar dynamics
Interface layer (scripting and high level languages)
Smoothed
particles
hydrodynamics
Metropolis
Hastings
Monte Carlo
Henyey
multi
-
shell
stellar evolution
4
th
order Hermite
block timestep
N
-
body
AMUSE
Limitations and Merits
-
Only problems whose physics are expressible
through module coupling (different time scales)
-
Low and high level use possible
-
Radiative transfer (and stellar evolution)
module links to VO (through eg. ‘spiegel’ and
‘partiview’): dust and stellar continuum, atomic
and molecular lines;
ELT, JWST, ALMA, Herschel
Impression of how it works
A)
install
B)
suite of test applications
C)
design your own multi
-
physics problem
D)
write script
E)
run
F)
analyze data
G)
download package from website
H)
write Nature paper
Design/Performance
AMUSE module must be written in language
with Foreign Function Interface (C, C++, Fortran
as well as high level languages like C#, Java,
Haskell. Low level applications optimized.
Top level uses a scripting language. These are
slow, but do just I/O, GUI, call sequence.
Top level can run in parallel (using MPI, GRID
technology); data exchange through HDF
Low level can run in parallel or on dedicated
hardware (eg GRAPE or GPU for direct N
-
body)
Initial Applications
Young and dense star cluster
Evolution of gas and stars near a black hole in
a galactic nucleus
Dynamics of embryonic planets in a debris disk
Relation to other projects
Different concept but with similar scientific
objectives/physics:
FLASH
Gadget
Starlab
Comparable in setup but with different scientific
objectives:
Atmosphere/Ocean/Tectonic
simulations by NASA
Molecular dynamics
QUESTIONS?
management/development plan
programmers under daily supervision of
software engineer and PI
regular interaction with
postdoc, who protects
scientific objectives
The cost
6
-
year of programming effort (3x2years?)
2 years of software engineering
2 years of postdoc
travel, webservices, hardware, etc.
total cost: 640Keuro
NOVA request: 500kEuro
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