![Page 1: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/1.jpg)
the theoretical understanding of
Type Ia Supernovae
Daniel Kasen
![Page 2: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/2.jpg)
Supernova Discovery History
Asiago Catalog (all supernova types)
SN cosmology“super-nova”
![Page 3: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/3.jpg)
Supernova FactoryLick observatory SN searchCfA SN groupCarnegie SN projectESSENCESupernova Legacy Survey
Supernova Discovery Future
Rough predictions and promises…
PanStarrsDark Energy SurveyJDEMLarge Synoptic Survey Telescope (LSST)
ProposedDark Energy Measurements
Systematic error, not statistical error, is the issue (e.g., luminosity evolution)
Aim for Type Ia SNe as reliable standard candles to a few %
![Page 4: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/4.jpg)
SN Ia ProgenitorsAccreting white dwarf near the Chandrasekhar
limit
Accretion rate:10-7 Msun / year
![Page 5: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/5.jpg)
White Dwarf IgnitionKuhlen, Woosley, and Glaitzmeier (2006)
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
![Page 6: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/6.jpg)
t = 0.0 sect = 0.5 sect = 1.0 sec
3D Deflagration ModelSubsonic turbulent flame burning
t = 1.5 sec
Roepke et al. (2005)
![Page 7: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/7.jpg)
C/O
boom
Fe
56Ni
Si/S/Ca
C/O
![Page 8: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/8.jpg)
Type Ia Supernova Light Curves
powered by the beta decay: 56Ni 56Co 56Fe
![Page 9: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/9.jpg)
Type Ia Supernova Spectrum
20 days after explosion
![Page 10: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/10.jpg)
Spectroscopic Homogeneity and Diversity
monitoring silicon expansion velocitiesfrom Leonard et al, ApJ 2006
![Page 11: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/11.jpg)
Type Ia Width-Luminosity Relation
brighter supernovae have broader light curves
![Page 12: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/12.jpg)
Supernova Ejecta Opacity
blending of millions of line transitions
FeII bound-boundFeIII bound-bound
![Page 13: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/13.jpg)
free expansion
Light Curves / Spectra(~100 days)
radioactive decay / radiative transfer
Type Iasupernovatheoreticalsimulation challenge
ignition
Presupernova Evolution(~100-109 years)
accreting, convective white dwarf
Explosion (~1-100 secs)
turbulent nuclear combustion / hydrodynamics
Observations
DOE: Scientific Discovery through Advanced Computing (SciDAC)
The “Computational Astrophysics Consortium” (CAC) Stan Woosley (PI)
UC Santa Cruz, UC Berkeley, Stanford, Arizona, Stony Brook, JHU,LANL, LLNL, LBNL
Models
![Page 14: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/14.jpg)
3-dimensional Time-Dependent Monte Carlo Radiative Transfer
SEDONA CodeExpanding atmosphereRealistic opacitiesThree-dimensionalTime-dependentMulti-wavelengthIncludes spectropolarizationIncludes radioactive decay and gamma-ray transferIterative solution for thermal equilibrium
Kasen et al 2006 ApJ
![Page 15: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/15.jpg)
Large Scale Computing
Jacquard, NERSC
Incite award, Oak Ridge Lab: 4 million hours/yearAtlas “grand challenge” LLNL: 4 million hours/yearNERSC award, LBL: 3 million hours/year
![Page 16: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/16.jpg)
Fe
56Ni
Si/S/Ca
C/OGrid of Type Ia Supernova Modelsw/ Stan WoosleySergei BlinikovElena Sorokina
130 one-dimensionalChandrasekhar massmodels with varied composition
ParametersMFe
MNi
MSi
“mixing”MFe + MNi + MSi + Mco = MCH
![Page 17: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/17.jpg)
Broadband Synthetic Light Curves
Model Compared to observations of SN 2001el
Kasen (2006) ApJ
ParametersMFe = 0.1 Msun MNi = 0.6 Msun
MSi = 0.4 Msun
Kasen, ApJ 2006
![Page 18: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/18.jpg)
Day 35 after explosion
Time Evolution of Spectrum
Recession of photosphere reveals deeper layers
Fe
56Ni
Si/S/Ca
C/ODay 15 after explosion
ModelSN1994D
![Page 19: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/19.jpg)
Width-Luminosity Relationship
Kasen and Woosley, ApJ, 2007 Vary 56Ni productionMNi = 0.35 to 0.70 Msun
![Page 20: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/20.jpg)
The Width-Luminosity Relationship
Kasen and Woosley, ApJ, 2007
Vary 56Ni production
Brighter models are hotter andmore ionized and have different opacity behavior
![Page 21: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/21.jpg)
The Width-Luminosity Relationship
Kasen and Woosley, ApJ, 2007
Vary 56Ni production
Vary silicon production(explosion energy)
![Page 22: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/22.jpg)
Multi-Dimensional Models
Roepke et al (2005)
![Page 23: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/23.jpg)
2D Deflagration Model
MNi = 0.2 Msun
EK = 0.3 x 1051 ergs
Roepke, Kasen, Woosley
![Page 24: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/24.jpg)
DeflagrationToDetonationKhokhlov (1991)Hoeflich (1994)Gamezo et al (2005)
But how to detonate?
Gamezo et al.
![Page 25: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/25.jpg)
2D Delayed Detonation
MNi = 0.5 Msun
EK = 1.2 x 1051 ergs
Roepke, Kasen, Woosley
Earlier Detonation (higher densities)gives more 56Ni production
![Page 26: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/26.jpg)
Off-Center Ignition
University of Chicago FLASH Center
![Page 27: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/27.jpg)
Detonation From Failed Deflagration Plewa, ApJ (2007)
Is the transition robust in3-dimensional calculations?
![Page 28: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/28.jpg)
Off-center ExplosionPlewa (2007) Kasen and Plewa (2007)
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
![Page 29: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/29.jpg)
Asymmetry and SN Ia Diversity
Maximum Light Spectrum
![Page 30: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/30.jpg)
Asymmetry and SN Ia Diversity
B-band Light Curve and the Phillips Relation
![Page 31: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/31.jpg)
How and where does ignition happen?
How might the deflagration transition into a detonation?
Can we reproduce the observed spectra and light curves from first principles?
How do the light curves depend upon progenitor environment?
Pressing Questions
The Theoretical Understanding of Type Ia Supernovae
![Page 32: the theoretical understanding of Type Ia Supernovae](https://reader038.vdocument.in/reader038/viewer/2022110211/5681308e550346895d966a62/html5/thumbnails/32.jpg)