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Supernova neutrino challengesSupernova neutrino challenges
Christian Y. Cardall
Oak Ridge National LaboratoryPhysics Division
University of Tennessee, KnoxvilleDepartment of Physics and Astronomy
Terascale Supernova Initiativehttp://www.phy.utk.edu/tsi
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Introduction to supernovaeIntroduction to supernovae
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Peter Apian, Cosmographia (1524)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Tycho Brahe, De Nova et Aevi Memoria Prius Visa Stella (1573)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Johannes Kepler, De Stella Nova in Pede Serpentarii, (1606)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
M31 (Andromeda Galaxy)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
SN 1987A
Tarantula Nebula
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
SN 1998aq(in NGC 3982)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
The name "supernova" dates from the 1930s.New stars or "novae" were well known.
The debate about the nature of spiral nebulae led to the realization that there must be
"giant novae" (Lundmark 1920),novae of "impossibly great absolute
magnitudes" (Curtis 1921),"exceptional novae" (Hubble 1929)"Hauptnovae" (Baade 1929).
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
The name "supernova" dates from the 1930s.The word "supernova" is claimed to have been
used by Baade and Zwicky since 1931.
LSN/LCN=103
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Spectral classification of supernovae:
Filippenko (1997)
Type II(obvious H)
Type I(no H)
Type Ia(no H, strong Si)
Type Ic(no H, He, Si)
Type Ib(no H, obvious He)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Physical classification of supernovae:Thermonuclear runaway;
Type Ia, accretion onto a white dwarf.
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Physical classification of supernovae:Core collapse of a massive star;
Type II, outer H layer remains at collapse;
Type Ib, outer H layer stripped before collapse;
Type Ic, outer H and He layers stripped before collapse.
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Neutrino predictions ca. 1986Energy release ~ 1053 erg in neutrinos,Emitted on a time scale of seconds,With an average neutrino energy of ~10 MeV
Burrows and Lattimer 1986
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
The lucky messengers…
Each “event” involves ~109 “messengers,”with at most 1 “detected”
SN1987A sent ~1058 “messengers,”with ~two dozen detected
Raffelt (1999)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Prediction vs. observationBurrows and Lattimer 1987
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
On the way to explosion…Accretion continues until stalled shock is
reinvigorated: relation between neutron star mass and delay to explosion
Optical display is powered by the decay of 56Ni; connection to neutrino transport
The electron fraction…
which determines how much 56Ni is produced is set by neutrino interactions:
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Dispersion of elements, electromagnetic display
Chandra X-ray Observatory (1999)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Chandra X-ray Observatory (2004)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Survey of collapse Survey of collapse simulationssimulations
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
The observables to understand includeExplosion (and energy thereof);Neutrinos;Remnant properties,
Mass, spin, kick velocity, magnetic fields;
Gravitational waves;Element abundances;Measurements across the EM spectrum,
IR, optical, UV, X-ray, gamma-ray;images, light curves, spectra, polarimetry...
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Some key ingredients are
Neutrino transport/interactions,
Spatial dimensionality;Dependence on energy and angles;Relativity;Comprehensiveness of interactions;
(Magneto)Hydrodynamics/gravitation,
Dimensionality;Relativity;
Equation of state/composition,
Dense matter treatments;Number and evolution of nuclear species;
Diagnostics,
Accounting of lepton number;Accounting of energy;Accounting of momentum.
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Simulations of collapse and explosionSpherical symmetry + mixing prescription,
simplified neutrino transport
Totani, Sato, Dalhed, & Wilson (1998)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
2S 0M
1S 1M
3S 0M
1S 2M
2S 1M
1.5 2M
S 3S 1M
2S 3M
N GR N GR N GR N GR N GR N GR N GR N GR
1S N
GR
2S N
B
GR
B
3S N
B
GR
B
Mag
neto
hydr
odyn
amic
sNeutrino radiation transport
Fluid mixing prescription in the coreboosts neutrino luminosities; notaccepted by most other investigators
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Simulations of collapse and explosionMultiple spatial dimensions, simplified neutrino
transport
Fryer & Warren (2002) Burrows, Hayes, & Fryxell (1995)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
2S 0M
1S 1M
3S 0M
1S 2M
2S 1M
1.5 2M
S 3S 1M
2S 3M
N GR N GR N GR N GR N GR N GR N GR N GR
1S N
GR
2S N
B
GR
B
3S N
B
GR
B
Mag
neto
hydr
odyn
amic
sNeutrino radiation transport
Neutron star mass too small; heating drives explosion too soon.
56Ni mass too small; Ye too low.
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Simulations of collapse and explosionMultiple spatial dimensions, simplified neutrino
transport
Janka & Mueller (1996)
Mezzacappa, Calder, Bruenn, Blondin, Guidry, Strayer, & Umar (1998)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
2S 0M
1S 1M
3S 0M
1S 2M
2S 1M
1.5 2M
S 3S 1M
2S 3M
N GR N GR N GR N GR N GR N GR N GR N GR
1S N
GR
2S N
B
GR
B
3S N
B
GR
B
Mag
neto
hydr
odyn
amic
sNeutrino radiation transport
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Simulations of collapse and explosionSpherical symmetry, sophisticated neutrino
transport
Rampp & Janka (2000)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Simulations of collapse and explosionSpherical symmetry, sophisticated neutrino
transport
Thompson, Burrows, & Pinto (2002)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
2S 0M
1S 1M
3S 0M
1S 2M
2S 1M
1.5 2M
S 3S 1M
2S 3M
N GR N GR N GR N GR N GR N GR N GR N GR
1S N
GR
2S N
B
GR
B
3S N
B
GR
B
Mag
neto
hydr
odyn
amic
sNeutrino radiation transport
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Simulations of collapse and explosionSpherical symmetry, sophisticated neutrino
transport
Liebendoerfer, Mezzacappa, Thielemann, Messer, Hix, & Bruenn (2001)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
2S 0M
1S 1M
3S 0M
1S 2M
2S 1M
1.5 2M
S 3S 1M
2S 3M
N GR N GR N GR N GR N GR N GR N GR N GR
1S N
GR
2S N
B
GR
B
3S N
B
GR
B
Mag
neto
hydr
odyn
amic
sNeutrino radiation transport
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Simulations of collapse and explosionMultiple spatial dimensions, intermediate neutrino
transport
Janka, Buras, & Rampp (2002)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
2S 0M
1S 1M
3S 0M
1S 2M
2S 1M
1.5 2M
S 3S 1M
2S 3M
N GR N GR N GR N GR N GR N GR N GR N GR
1S N
GR
2S N
B
GR
B
3S N
B
GR
B
Mag
neto
hydr
odyn
amic
sNeutrino radiation transport
Neutron star mass and 56Ni mass are reasonable.
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
The Terascale Supernova The Terascale Supernova InitiativeInitiative
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
A diverse and experienced investigator team...
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
...with expertise in all necessary areas...Radiation transport,
(Magneto-)hydrodynamics,
Nuclear and weak interaction physics,
Computer science,Large sparse linear systems,
Data management and visualization;
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
...and support from the U.S. Department of Energy:Funding through the DOE Office of Sciences'
SciDAC program,
Access to DOE's terascale machines (several 1012 bytes of memory and flops),
Access to the expertise of teams specializing inAdvanced solvers,
Advanced computational meshes,
Performance on parallel architectures,
Data management and visualization,
Software interoperability and reusability.
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Accretion shock instabilityA standing accretion shock, an analytic solution in
spherical symmetry, is used as an initial condition.
Blondin, Mezzacappa, & DeMarino (2003)
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Accretion shock instabilityThe standing accretion shock
is unstable in 2D/3D to thepoint of explosion.
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
QuickTime™ and aVideo decompressorare needed to see this picture.
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Neutrino radiation transport: a computational challenge
Large dynamic range in time and spaceTime scale of neutrino interactions is many
orders of magnitude smaller than the fluid time scale
Use implicit time differencing: Evaluate right-hand side at new values of the variables
Gravitational collapse gives a range of spatial scalesSome features need higher resolution, e.g. shock
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Neutrino radiation transport: a computational challenge
Dimensionality
2D: solution vector of several 109 elements3D: solution vector approaching 1012 elements
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
2S 0M
1S 1M
3S 0M
1S 2M
2S 1M
1.5 2M
S 3S 1M
2S 3M
N GR N GR N GR N GR N GR N GR N GR N GR
1S N
GR
2S N
B
GR
B
3S N
B
GR
B
Mag
neto
hydr
odyn
amic
sNeutrino radiation transport
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Adaptive mesh refinement
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
Supernova neutrino challengesSupernova neutrino challenges
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Supernova neutrino challengesChristian Y. CardallNOW2004, Conca Specchiulla, Italy, 11-17 September 2004
ProgenitorsTheory
Dense matter equation of stateNeutrino interactions with nuclei, dense matterNeutrino transport with flavor mixing, collisions,
time and space dependence
ComputationSpatially multidimensional, energy- and angle-
dependent, implicit neutrino transportInclusion of physics: magnetic fields, general
relativity, nuclear reaction networksObservation (talks by M. Selvi and A. Mirizzi this afternoon)
Large detectorsSignal expectations