morning afternoon mon. introduction to enzo tue. …hipacc.ucsc.edu/html/hipacclectures/enzo...
TRANSCRIPT
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Morning Afternoon
Mon. Introduction to Enzo
Tue. 1. Setting Up and Running Enzo2. Enzo Projects
Introduction to YT
Wed. Enzo Algorithms Lab session
Thu. Applications to First Stars, First Galaxies, and Reionization
Lab session
Fri. What’s New in Enzo 2.0? Q & A
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Feature Authors
physics
star particle class John Wise, Ji-hoon Kim
adaptive ray tracing radiative transfer John Wise, Tom Abel
flux limited diffusion radiative transfer Dan Reynolds
Runge-Kutta2 MHD Tom Abel, Peng Wang
CUDA MHD Tom Abel, Peng Wang
high-density primordial chemistry Matt Turk
CLOUDY cooling Britton Smith
sink particles John Wise, Peng Wang, Tom Abel
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Feature Authors
numerics
particle splitting Ji-hoon Kim
shearing box boundary conditions Tom Abel, Fen Zhao
inline Friends-Of-Friends John Wise
mpgraphic initial conditions John Wise
non-blocking communication John Wise, Greg Bryan
AMR checkpoint dumps Matt Turk
r16 Positioning Matt Turk
Python embedding Matt Turk
LCA-perf James Bordner
New Streaming Format John Wise, Tom Abel
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V1.5
V2.0
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I. Radiative Transfer with Ray TracingII. Radiating “Star” Particles
John Wise (Princeton)Enzo WorkshopUCSD – 29 Jun 2010
Tuesday, 29 June 2010
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Cosmological Radiative Transfer Equation
n := normal vectora := scale factorā := a/aem
H := Hubble factorν := frequency
Iν ≡ I(ν,x,Ω, t)
1c
∂Iν
∂t+
n ·∇Iν
a− H
c
ν
∂Iν
∂ν− 3Iν
= −κνIν + jν
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Cosmological Radiative Transfer Equation
n := normal vectora := scale factorā := a/aem
H := Hubble factorν := frequency
Iν ≡ I(ν,x,Ω, t)
Propagation &
Cosmic Expansion
Redshifting
Cosmological DilutionAbsorptionEmission
1c
∂Iν
∂t+
n ·∇Iν
a− H
c
ν
∂Iν
∂ν− 3Iν
= −κνIν + jν
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1c
∂Iν
∂t+
n ·∇Iν
a− H
c
ν
∂Iν
∂ν− 3Iν
= −κνIν + jν
Simplifications – “Local” Approximation
Propagation &
Cosmic Expansion
Redshifting
Cosmological DilutionAbsorptionEmission
1. Short timesteps (ā = 1)2. Ignore cosmological redshift and dilution (may
become important >50 Mpc)
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1c
∂Iν
∂t+
n ·∇Iν
a− H
c
ν
∂Iν
∂ν− 3Iν
= −κνIν + jν
Simplifications – “Local” Approximation
Propagation &
Cosmic Expansion
Redshifting
Cosmological DilutionAbsorptionEmission
1. Short timesteps (ā = 1)2. Ignore cosmological redshift and dilution (may
become important >50 Mpc)
Tuesday, 29 June 2010
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1c
∂Iν
∂t+
n ·∇Iν
a− H
c
ν
∂Iν
∂ν− 3Iν
= −κνIν + jν
Simplifications – “Local” Approximation
Propagation &
Cosmic Expansion
Redshifting
Cosmological DilutionAbsorptionEmission
1. Short timesteps (ā = 1)2. Ignore cosmological redshift and dilution (may
become important >50 Mpc)
Tuesday, 29 June 2010
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RT Equation along a Ray
• Consider point sources of radiation
• Initially, the radiation flux is split equally among all rays.
1c
∂P
∂t+
∂P
∂r= −κP
• P := photon flux in the ray
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Adaptive Ray TracingAbel & Wandelt (2002)
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Adaptive Ray TracingAbel & Wandelt (2002)
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Adaptive Ray TracingAbel & Wandelt (2002)
• Ray directions and splitting based on HEALPix (Gorski et al. 2005)
• Rays are split into 4 child rays when the solid angle is large compared to the cell face area
• Well-suited for AMR
• Fully coupled to the chemistry and energy solvers in Enzo, i.e. radiation hydrodynamics!
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Adaptive Ray TracingAbel & Wandelt (2002)
• Each ray is mono-chromatic
• Hydrogen ionizing (E > 13.6 eV)
• Helium singly ionizing (E > 24.6 eV)
• Helium doubly ionizing (E > 54.4 eV)
• X-rays• hydrogen ionizations• secondary ionizations• helium ionizations• reduced photo-heating
• H2 dissociating (Lyman-Werner)
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Time for an example!
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Cosmological RT Codes ComparisonIliev et al. (2006)
Test 1Source at the originUniform density fieldNo hydrodynamics
IsothermalMono-chromatic spectrum (13.6 eV)
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PhotonTest, i.e. CollapseTest with radiation sources
Turn on radiative transfer
Must be ≥1. Doesn’t make sense for an equation of
state (no ionizations)
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Minimum rays per cell, i.e. angular resolution
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Minimum rays per cell, i.e. angular resolution
Initial number of rays from the pt. source. N0 = 12 x 4n
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Minimum rays per cell, i.e. angular resolution
Initial number of rays from the pt. source. N0 = 12 x 4n
Determines timestep by restricting HI fraction change to 5%. Not stable for
big runs (yet).
If set to 0, uses hydro timestep on the finest level.
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Minimum rays per cell, i.e. angular resolution
Initial number of rays from the pt. source. N0 = 12 x 4n
Determines timestep by restricting HI fraction change to 5%. Not stable for
big runs (yet).
If set to 0, uses hydro timestep on the finest level.
If set to 1, uses one of the two timestepping schemes above.
If set to 0, uses constant (can be user-defined in dtPhoton).
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Number of point sources
SpheresSame parameters as CollapseTest
but replace with PhotonTest
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Number of point sources
For future use.
SpheresSame parameters as CollapseTest
but replace with PhotonTest
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Number of point sources
For future use.
(x,y,z) Must be in domain
SpheresSame parameters as CollapseTest
but replace with PhotonTest
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Number of point sources
For future use.
(x,y,z) Must be in domain
Total photon luminosity (ph/sec)
SpheresSame parameters as CollapseTest
but replace with PhotonTest
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Number of point sources
For future use.
(x,y,z) Must be in domain
Total photon luminosity (ph/sec)
Source lifetime in code units
SpheresSame parameters as CollapseTest
but replace with PhotonTest
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Number of point sources
For future use.
(x,y,z) Must be in domain
Total photon luminosity (ph/sec)
Source lifetime in code units
Energy of rays in energy group
SpheresSame parameters as CollapseTest
but replace with PhotonTest
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Cosmological RT Codes Comparison IIIliev et al. (2009)
Test 6 (with AMR)Source at the origin1/r2 density profileHydrodynamics
Blackbody spectrum (105 K)
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Turn hydro on
AMR with 2 levels
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Background temperature and electron fraction
No gravity (in accordance to the test parameters)
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Sphere parametersType 5 := 1/r2 density profile
with a core
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Density
Temperature
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How do I have >1 energy group?
Example:105 K blackbody in
4 energy groups
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How do I have >1 energy group?
Example:105 K blackbody in
4 energy groups
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How do I have >1 energy group?
Example:105 K blackbody in
4 energy groups
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How do I have >1 energy group?
Example:105 K blackbody in
4 energy groups
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Radiative “Star” Particles Complex behavior encouraged!
made with yt!
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Star particle overview
• Two types of star particles: (1) Normal and (2) Radiative
• Normal star particles are similar to DM particles but have particle attributes
• Creation time
• Dynamical time (or lifetime)
• Metallicity
• Normal star particles only interact with local grid cells.
• Feedback is accomplished through energy injection
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Star class
• To mirror nature better, star particles needed more flexibility.
• The class is an additional layer on top of the normal star particle, so it is included in the gravity solver and refinement criteria.
• Main advantage: greater interactivity between the stars and grid
• Able to change cells on multiple grids and levels
class Star ;
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Feedback spheres
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Star class
• Different types of feedback modes (all operate in spheres of any radius)
• Star formation – instantaneous accretion
• Supernova feedback – thermal energy injection
• Strömgren sphere – radial profile taken from Whalen et al. (2004)
• Color field – Marks sphere with a color
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Star class
• Can represent a single star, star cluster, black hole, neutron star, etc.
• Can grow from a pre-determined accretion rate “future”.
• Easy to merge.
• Doesn’t necessarily creates radiation. This is determined in Star_IsARadiationSource.C.
if (Star1->Mergable(Star2)) Star1 += Star2; Star2->DisableParticle(LevelArray);
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StarParticleIntitialize
StarParticleFinalize
StarParticleAddFeedback
Loop over all stars
StarParticleDeath
Loop over all stars
For each star
EvolveLevel
if first timestep
after restart
Main grid loop
in EvolveLevelCommunicationUpdateStarParticleCount
grid::FindAllStarParticles
Converts ALL active star particles into objects
yes
StarParticleFindAll
Update position and velocity of existing star objects.
Converts NEW star particles into star objects.
Creates a global list of star objects on all processors.
no
Synchronize stars in global list with copies in grids
StarParticleMergeNew
Merges NEW particles within some radius and the same type.
Delete merged particles.
Star::SetFeedbackFlag
Star::UpdatePositionVelocity
Copies new position and velocity from star particles to objects
if grid
feedback necessary
StarParticleAccretion
(for every star)
Calculate its mass accretion rate.
Add mass to star.
Star::HitEndPoint
if kill only star object
(e.g. active to inactive star)
delete only the star object.
ActivateNewStar
If star is now 'active'
(e.g. surpassed some mass threshold),
activate it by setting the type to positive.
ResetAccretion
Synchronize star in global list with copy in grids
Delete global star list.
next star
no
Star::CalculateFeedbackParameters
Calculates radius, density, color,
and energy of the feedback sphere.
yes
Star::FindFeedbackSphere
Determines whether the sphere is
enclosed in grids on the current level.
if sphere contained
no
grid::AddFeedbackSphere
Adds feedback sphere to grid.
yes
if supernova,
set FeedbackFlag to DEATH
if kill star
delete the star particle AND object.
http://lca.ucsd.edu/projects/enzo/wiki/Tutorials/StarParticleClass
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StarParticleIntitialize
StarParticleFinalize
StarParticleAddFeedback
Loop over all stars
StarParticleDeath
Loop over all stars
For each star
EvolveLevel
if first timestep
after restart
Main grid loop
in EvolveLevelCommunicationUpdateStarParticleCount
grid::FindAllStarParticles
Converts ALL active star particles into objects
yes
StarParticleFindAll
Update position and velocity of existing star objects.
Converts NEW star particles into star objects.
Creates a global list of star objects on all processors.
no
Synchronize stars in global list with copies in grids
StarParticleMergeNew
Merges NEW particles within some radius and the same type.
Delete merged particles.
Star::SetFeedbackFlag
Star::UpdatePositionVelocity
Copies new position and velocity from star particles to objects
if grid
feedback necessary
StarParticleAccretion
(for every star)
Calculate its mass accretion rate.
Add mass to star.
Star::HitEndPoint
if kill only star object
(e.g. active to inactive star)
delete only the star object.
ActivateNewStar
If star is now 'active'
(e.g. surpassed some mass threshold),
activate it by setting the type to positive.
ResetAccretion
Synchronize star in global list with copy in grids
Delete global star list.
next star
no
Star::CalculateFeedbackParameters
Calculates radius, density, color,
and energy of the feedback sphere.
yes
Star::FindFeedbackSphere
Determines whether the sphere is
enclosed in grids on the current level.
if sphere contained
no
grid::AddFeedbackSphere
Adds feedback sphere to grid.
yes
if supernova,
set FeedbackFlag to DEATH
if kill star
delete the star particle AND object.
http://lca.ucsd.edu/projects/enzo/wiki/Tutorials/StarParticleClass
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Radiative Star Particles
• Population III stars – method 3. Represent single Pop III stars. Luminosity, lifetime, and endpoint determined from PopIIIStarMass
• “Star cluster” particles – method 5. Represents a star cluster or galaxy (depending on resolution).
• In Enzo 2.0, multiple star formation routines may be used.
• Specified in a bitwise fashion. • Method 3 → 23 = 8• Method 4 → 24 = 16• Method 3 & 5 → 23 + 25 = 40
• Black hole particles – PopIIIBlackHoles = 1
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Metal enrichment
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Metal enrichment
Minimum tdyn of a star-forming molecular cloud (higher → lower
dens. & more massive). In years.
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Metal enrichment
Minimum tdyn of a star-forming molecular cloud (higher → lower
dens. & more massive). In years.
Ionizing photons / sec / M⊙
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Metal enrichment
Minimum tdyn of a star-forming molecular cloud (higher → lower
dens. & more massive). In years.
Ionizing photons / sec / M⊙
Use helium ionizing photons
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Metal enrichment
Minimum tdyn of a star-forming molecular cloud (higher → lower
dens. & more massive). In years.
Ionizing photons / sec / M⊙
Use helium ionizing photons
SN energy – erg / M⊙
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Metal enrichment
Minimum tdyn of a star-forming molecular cloud (higher → lower
dens. & more massive). In years.
Ionizing photons / sec / M⊙
Use helium ionizing photons
SN energy – erg / M⊙
Radius (pc) to inject SN feedback thermal energy. In the code, minimum of 3.5 cell widths.
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Metal enrichment
Minimum tdyn of a star-forming molecular cloud (higher → lower
dens. & more massive). In years.
Ionizing photons / sec / M⊙
Use helium ionizing photons
SN energy – erg / M⊙
Radius (pc) to inject SN feedback thermal energy. In the code, minimum of 3.5 cell widths.
Star formation efficiency. This fraction of the cold gas mass is
converted into a star.
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Metal enrichment
Minimum tdyn of a star-forming molecular cloud (higher → lower
dens. & more massive). In years.
Ionizing photons / sec / M⊙
Use helium ionizing photons
SN energy – erg / M⊙
Radius (pc) to inject SN feedback thermal energy. In the code, minimum of 3.5 cell widths.
Star formation efficiency. This fraction of the cold gas mass is
converted into a star.
Star cluster minimum mass (M⊙)
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Metal enrichment
Minimum tdyn of a star-forming molecular cloud (higher → lower
dens. & more massive). In years.
Ionizing photons / sec / M⊙
Use helium ionizing photons
SN energy – erg / M⊙
Radius (pc) to inject SN feedback thermal energy. In the code, minimum of 3.5 cell widths.
Star formation efficiency. This fraction of the cold gas mass is
converted into a star.
Star cluster minimum mass (M⊙)
Radius (pc) to combine stars when first created
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Stellar mass in M⊙ (constant)
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Stellar mass in M⊙ (constant)
Use radiative BH particles when <140 M⊙ and >260 M⊙ stars
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Stellar mass in M⊙ (constant)
Use radiative BH particles when <140 M⊙ and >260 M⊙ stars
LBH = f * dMBH/dt * c2
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Stellar mass in M⊙ (constant)
Use radiative BH particles when <140 M⊙ and >260 M⊙ stars
LBH = f * dMBH/dt * c2
Overdensity to form StarCluster and Pop III star particles
(negative value for units of cm-3)
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Stellar mass in M⊙ (constant)
Use radiative BH particles when <140 M⊙ and >260 M⊙ stars
LBH = f * dMBH/dt * c2
Overdensity to form StarCluster and Pop III star particles
(negative value for units of cm-3)
Minimum H2 fraction to form
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Stellar mass in M⊙ (constant)
Use radiative BH particles when <140 M⊙ and >260 M⊙ stars
LBH = f * dMBH/dt * c2
Overdensity to form StarCluster and Pop III star particles
(negative value for units of cm-3)
Minimum H2 fraction to form
Maximum metallicity (in absolute, not solar, fractions) of Pop III stars
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Stellar mass in M⊙ (constant)
Use radiative BH particles when <140 M⊙ and >260 M⊙ stars
LBH = f * dMBH/dt * c2
Overdensity to form StarCluster and Pop III star particles
(negative value for units of cm-3)
Minimum H2 fraction to form
Maximum metallicity (in absolute, not solar, fractions) of Pop III stars
Radius (pc) to inject SN energy
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Stellar mass in M⊙ (constant)
Use radiative BH particles when <140 M⊙ and >260 M⊙ stars
LBH = f * dMBH/dt * c2
Overdensity to form StarCluster and Pop III star particles
(negative value for units of cm-3)
Minimum H2 fraction to form
Maximum metallicity (in absolute, not solar, fractions) of Pop III stars
Radius (pc) to inject SN energy
Use a color (metal) field in SN feedback
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Stellar mass in M⊙ (constant)
Use radiative BH particles when <140 M⊙ and >260 M⊙ stars
LBH = f * dMBH/dt * c2
Overdensity to form StarCluster and Pop III star particles
(negative value for units of cm-3)
Minimum H2 fraction to form
Maximum metallicity (in absolute, not solar, fractions) of Pop III stars
Radius (pc) to inject SN energy
Use a color (metal) field in SN feedback
Use at your own risk. Pre-refines region before supernova.
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Let’s put them together.
+
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Toy ReionizationSimulation
• 30 Mpc, 643 resolution
• AMR with 8 levels
• Maximal spatial resolution of 1.8 comoving kpc
• 4 x 109 M⊙ DM mass resolution
• Hydrogen ionization only
• Star cluster particles with metal enrichment
• Stop at z = 6
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No full reionization because of mass resolution (i.e. we miss all of the low-luminosity dwarfs)
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Create your own star particle type
1. In macros_and_parameters.h, add your particle type macro.
2. Add a “star_maker” to Grid_StarParticleHandler.C or create your own routine that adds particles to the grid (e.g., only done in a restart).
• Assign the new particles a particle type = –NEW_PARTICLE_TYPE, which tells the Star class routines to create a new Star object from this particle. It will be changed into a positive number when the Star object is created.
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Create your own star particle type
3. Add your new star particle type to the if-statement in Grid_FindNewStarParticles.C
4. Add a case-statement to Star_SetFeedbackFlag
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Create your own star particle type
3. Add your new star particle type to the if-statement in Grid_FindNewStarParticles.C
4. Add a case-statement to Star_SetFeedbackFlag
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Create your own star particle type
5. If adding a feedback sphere, you can customize your own sphere in
Star_CalculateFeedbackParameters.C
Grid_AddFeedbackSphere.C.
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Create your own star particle type
6. Add a case-statement to Star_ActivateNewStar.C
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Create your own star particle type
7. If you don’t want your new star particle type to be radiating (i.e. only add feedback spheres), add an additional logic check in Star_IsARadiationSource.C.
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Summary
• Run non-cosmological radiative hydrodynamics problems.
• New Star class
• New “star cluster” and Population III star particles.
• Run cosmological simulations with radiation transport from dynamically created star particles
• Create your own radiating “star” particle type.
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Self-consistent Cosmological Radiation Hydrodynamics/Ionization
• implicit flux limited diffusion solver• coupled to ionization kinetics and gas energy equation• only for unigrid in 2.0 (AMR not supported yet)• requires hypre library from LLNL
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Self-consistent Cosmological Radiation Hydrodynamics/Ionization
Reynolds, Hayes, Paschos & MN (2009)• Goal
– Create a parallel scalable solver that couples cosmological hydrodynamics, radiation transport, chemical ionization, and gas photoheating self-consistently
Explicit cosmological hydrodynamics
(ENZO)
Implicit radiation transport, ionization
kinetics, and photoheating
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Cosmological Radiative Transfer Equation
EcEE
a
a
a
F
t
E
dnnIFdnIc
E
zta
III
c
tH
a
In
t
I
c
4)3(
ˆ)ˆ( ;)ˆ(1
factor scale cosmic 1
1)(
)3()(ˆ1
2
Spatial gradients WRT coordinates comoving with expanding universe
cosmological
redshift
cosmological
expansion
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EcEEa
aED
aE
aE bt 43)(
1)(
12
Reduces to standard equation setting a=1
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Spectral Modeling: 1-group Approximation
)/(
)(B
)(
)(
00
0
powerlaw
blackbody
ticmonochroma
TE
Comoving radiation energy density
EcEa
amED
aE
aE bt 4)(
1)(
12
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Why use FLD?
• Invented by my thesis adviser Jim Wilson
• Simple and easy (no formal solution needed)
• Correct behavior in limiting regimes
• Causal propagation of radiation energy
• I am interested in large volumes and many sources, where diffuse radiation backgrounds dominate local effects (i.e., shadows)
• SPD matrixefficient solution methods
• Extenstion to VTEF with analytic EFs straightforward
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System of Equations
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Operator Splitting
ionizationradiation/ with coupling todue correctionenergy is
motions ichydrodynam todueenergy gas is
where
let
c
h
ch
e
e
eee
Gas energy equation
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Explicit hydrodynamics
This is what ENZO already does
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Implicit Coupled System
• non-equilibrium multispecies model
• LTE (2 temperature) model
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Temporal DiscretizationGeneralized Crank-Nicholson (theta scheme)
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Multigrid-Preconditioned Conjugate Gradient
• The primary difficulty in solving these systems lies in the Schur complement system
(D – LM-1U) xE = bE – LM-1bM
• Due to the diffusion approximation, and the spatial locality of M and L, this matrix is symmetric and positive definite.
• SPD systems are often solved using the conjugate-gradient method; a robust, low-memory Krylov iterative solver. Unfortunately, CG convergence rates depend on the eigenvalues of the matrix, which here spread rapidly with mesh refinement, resulting in slower convergence as the mesh is refined.
• We therefore precondition the CG solver, i.e. Ax = b (P-1AP-1)(Px) = P-1b, where the symmetric operator P-1 comes from a geometric multigrid (MG) solver.
• MG methods, while less robust, exhibit convergence rates that are independent of the matrix spectrum, resulting in near optimal log-linear algorithm complexity, and scalability to thousands of processors.
• This MG-CG combination results in a robust, scalable solver for the inner Schur systems.
HYPRE solver library, LLNL
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Build Configuration
To use any FLD solver module, Enzo must be configured with:
gmake photon-yes [enables all radiation solvers]gmake hypre-yes [enables HYPRE solver interface]gmake use-mpi-yes [enables MPI]
Moreover, the machine Makefile must specify how to include andlink with an available HYPRE library (version ≥ 2.4.0b).
If you must compile HYPRE yourself, use the configuration option--with-no-global-partition for runs using over 1000 tasks.
Optional/recommended Enzo configuration options include:
gmake emissivity-yes [enables coupling with star-maker]gmake precision-64 [the solvers prefer double precision]
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Startup Parameters
The main problem parameter file must have the following parameters:
RadiativeTransferFLD [0] – this must be 2.
ImplicitProblem [0] – use 3 for gFLDSplit, 1 for gFLDProblem.
ProblemType [0] – FLD-based solvers use values in the 400’s.
RadHydroParamfile [NULL] – the filename containing allFLD-specific solver parameters (next slide).
RadiativeTransferOpticallyThinH2 [1] – this must be 0.
RadiationFieldType [0] – can be any value except 10 or 11.
RadiativeTransferFLDCallOnLevel [0] – must currently be 0.
RadiativeTransfer [0] – this must be be 0.
RadiativeCooling [0] – must currently be 0.
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FLD Solver Parameters (separate input file)
The following parameters control various aspects of gFLDSplit:
RadHydroESpectrum [1] – form for radiation spectrum χE (ν):
-1. is monochromatic at hν = 13.6 eV,0. is power law,1. is T = 105 blackbody.
RadHydroChemistry [1] – controls whether to use nHI (1 yes, 0 no)
RadHydroHFraction [1] – controls the fraction of baryonic mattercomprised of Hydrogen (RadHydroHFraction ∈ [0, 1]).
RadHydroModel [1] – determines which model for radiation-mattercoupling we wish to use:
1. Chemistry-dependent model with case B recombination coeff.4. Same as model 1, with an isothermal gas energy.
10. Local thermodynamic equilibrium model (no nHI ).
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FLD Solver Parameters – continued
RadHydroMaxDt [1020] – sets ∆tmax in scaled time units.
RadHydroMinDt [0] – sets ∆tmin in scaled time units.
RadHydroInitDt [1020] – sets the initial ∆tE in scaled time units.
RadHydroDtNorm [2] – sets p in computing the time error estimate.
RadHydroDtRadFac, RadHydroDtGasFac, RadHydroDtChemFac[1020] – the values of τi,tol in computing ∆tE , ∆te and ∆tHI .
RadiationScaling, EnergyCorrectionScaling,ChemistryScaling [1.0] – the scaling factors sE , se and sn.
RadHydroTheta [1.0] – the ∂tE discretization parameter, θ.
RadHydroSolTolerance [10−8] – linear solver tolerance δ.
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FLD Solver Parameters – continued
RadiationBoundaryX0Faces, RadiationBoundaryX1Faces,RadiationBoundaryX2Faces [0 0] – BC types at each face:
0. periodic (must match on both faces in a given direction)1. Dirichlet2. Neumann
EnergyOpacityC0-EnergyOpacityC2 [1, 1, 0] – theopacity-defining constants C0-C2 for the LTE model.
RadHydroMaxMGIters [50] – max number of MG-CG iterations.
RadHydroMGRelaxType [1] - the MG relaxation method:
0. Jacobi1. Weighted Jacobi2. Red/Black Gauss-Seidel (symmetric)3. Red/Black Gauss-Seidel (nonsymmetric)
RadHydroMGPreRelax [1] – number of pre-relaxation MG sweeps.
RadHydroMGPostRelax [1] – number of post-relaxation MG sweeps.
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Customization
To set up a new FLD problem:
Allocate a baryon field with FieldType set to RadiationFreq0.
Set η(x, t) by either:
Edit gFLDSplit RadiationSource.src90 orgFLDProblem RadiationSource.src90,
Fill in the baryon field Emissivity0, and edit logic ingFLDSplit Evolve.C or gFLDProblem Evolve.C to use thatfield (emulate logic for StarMakerEmissivityField).
Edit gFLDSplit Initialize.C or gFLDProblem Initialize.C tocall the problem initializer and set BCs.
All other requirements for setting up a new ProblemType in Enzo arelike normal (InitializeNew.C, problem initialization files, etc.).
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Iliev Test 5 Example – Dynamic I-front Expansion
[on Triton: /home/enzo-1/IlievEtAl5]
Dynamic ionization test of an initially-neutral hydrogen region:
Box size L = 15 kpc; Run time Tf = 500 Myr.
T = 105 blackbody spectrum, at rate Nγ = 5 · 1048 photon/s.
Initial conditions: n = 10−3 cm−3, T = 100 K, E = 10−30 erg
cm3 .
No available analytical solution, but:
Front transitions from R- to D-type as it reaches Stromgren radius,
rRI = rS
[1− e−tαB (Ti )nH
]1/3
, rDI = rS [1 + (7cst)/(4rS)]4/7
,
Eventually stalls at rf = rS(
2Ti
Te
)2/3
, where Ti and Te are the
temperatures behind and ahead of the I-front.
[Whalen & Norman, ApJS, 2006; Iliev et al., MNRAS, 2009]
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Hydrodynamic Radiative Ionization Results
0 0.5 1 1.5 2 2.5 3 3.5 4 4.50
0.5
1
1.5
2
2.5
t/trec
r I/r S
Convergence in I−front Position
163 mesh323 mesh643 mesh1283 mesh
0 0.5 1 1.5 2 2.5 3 3.5 4 4.50
0.005
0.01
0.015
0.02
0.025
0.03
0.035
0.04
0.045
t/trec
|r I−r I* |/r
S
Error in I−front Position
163 mesh323 mesh643 mesh
NW:I-front position history
NE:T profile (175 Myr)
SW:rI conv. wrt ∆x
SE:T convergence wrt ∆t
0 0.2 0.4 0.6 0.8 11.5
2
2.5
3
3.5
4
4.5
r/Lbox
log(
T)
Temperature profile, t = 175 Myr
0 0.1 0.2 0.3 0.4 0.510−8
10−7
10−6
10−5
10−4
10−3
10−2
10−1
r/Lbox
rela
tive
erro
r
Temperature error profile, t = 175 Myr
5e−42e−41e−45e−52e−51e−5
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Shapiro & Giroux [Isothermal, Static Cosmic Ionization]
[in enzo-2.0: run/RadiationTransportFLD/SG q5z4 sp]
Repeat of previous test, but in a cosmologically expanding universe, witha static, isothermal gas, using a monochromatic radiation spectrum.
Four tests:q0 zi Li [kpc] ρb,i [g cm−3] H0 Ωm ΩΛ Ωb
0.5 4 80 1.18e-28 0.5 1.0 0 0.20.05 4 60 2.35e-28 1.0 0.1 0 0.10.5 10 36 1.18e-28 0.5 1.0 0 0.20.05 10 27 2.35e-28 1.0 0.1 0 0.1
Analytical solution given by
rI (t) = rS,i
(λe−τ(t)
∫ a(t)
1
eτ(b)[1− 2q0 + 2q0(1 + zi )/b]−1/2db
)1/3
,
τ(a) = λ [F (a)− F (1)][6q2
0(1 + zi )2]−1
, λ =αBnH,i
H0(1+zi ),
F (a) =[2− 4q0 − 2q0
1+zi
a
] [1− 2q0 + 2q0
1+zi
a
]1/2.
[Shapiro & Giroux, ApJ, 1987]
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Cosmological Ionization Results
0 0.5 1 1.5 2 2.5 30
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1
−log[(1+z)/(1+zi)]
r/rs
ri(t)/rs(t) vs redshift
q0=0.5, z0=4q0=0.05, z0=4q0=0.5, z0=10q0=0.05, z0=10
−0.1 0 0.1 0.2 0.3 0.4 0.5 0.6 0.7−0.1
0
0.1
0.2
0.3
0.4
0.5
0.6
−log[(1+z)/(1+zi)]
r/rs
ri(t)/rs(t) vs redshift, zi=4
q0=0.5 (computed)q0=0.5 (analytic)q0=0.05 (computed)q0=0.05 (analytic)
NW:I-front radii vs scaled z
NE:I-front error vs scaled z
SW:I-front radii for zi = 4.
SE:Weak CPU scaling(Nsrc ∝ NCPU)
Kraken @ NICS:O(N log N) scaling
0 0.1 0.2 0.3 0.4 0.5 0.6 0.71
2
3
4
5
6
7
8
9
10
11x 10−3
−log[(1+z)/(1+z0)]
(r true−
r)/r s
Error in ri(t)/rs(t) vs scaled redshift, q0 = 0.5, z0 = 4
163 mesh323 mesh643 mesh
1 8 64 512 4096 327685
10
15
20
25
Cores
Aver
age
wall t
ime
/ ste
p (s
)
Cosmology Weak Scaling (Kraken): Tavg vs Cores
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Reionization Simulations (FLD + StarMaker)
[in enzo-2.0: run/RadiationTransportFLD/CosmologyFLD RT]
Geoffrey So has constructed an interface to StarMaker to seed η(x, t):
Requires Enzo configuration with EMISSIVITY enabled,
Adds StarMakerEmissivityField=1 to main parameter file,
The interface fills the Emissivity0 baryon field based on emissionfrom star particles; the FLD modules copy this field into η(x, t).
Utilizes identical startup machinery as typical cosmology runs, viaCosmologySimulationInitialize.C [ProblemType 30], withadditional input file options to enable the FLD solver module.
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Reionization Simulations (FLD + StarMaker)
ρ
E
xHI
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Summary of Current Results
The gFLDSplit and gFLDProblem solver modules implement a grey,field-based, flux-limited diffusion radiation approximation for unigrid runs:
Implicit MG-CG solvers enable scalable solution on many thousandsof cores, independently of the number of ionization sources.
Accurately solves couplings between radiation, ionization and gasenergy, due to implicit formulation and coupled solvers.
Split and implicit formulations allow for tradeoffs betweenrobustness/efficiency and accuracy.
However, this approximation has its shortcomings:
Single radiation field allows full absorption by hydrogen, eventhough higher-frequency radiation should pass through.
Though better than simpler approximations, grey approach cannotaccurately handle multi-species problems (hence H-only restriction).
Currently limited to unigrid Enzo simulations.