surviving companions of type ia supernovaebps.ynao.cas.cn/xzzx/201908/w020190820419297892052.pdf ·...
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Surviving Companions of Type Ia Supernovae
Callum McCutcheon
Yunnan Observatories,
University of Surrey
Collaboration with Zhengwei Liu, Zhanwen Han, Xuefei Chen, Hai-Liang Chen, Kuo-Chuan Pan
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Background
• Competing theories for Type Iageneration• Single-degenerate – WD +
MS/RG/He
• Double-degenerate – WD + WD (WD+NS/BH)
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Background – SD channel
• SD will leave behind companion star (remnants!) – potential method to discern between the channels
• Properties of surviving star could help to determine properties of binary system before explosion• Kick velocity
• Heavy element distribution
• Simulate impact of ejecta on companion
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Changing explosion model
Pan, Ricker, Taam, ApJ, 2014
• Hard to reconcile SD scenario with surviving companion candidates after long-term evolution (SN 1572, SN 1006, SNR 0519-69)
• If changing companion star model does not quite fit, try changing explosion model!
• Explosion models differ in abundance spatial distribution, velocity, etc.
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Hydrodynamic codes - approaches
• Two main approaches – Grid/SPH
FLASH - Grid-basedHighly modular AMR grid-based code
Can be adapted for different solving regimes, grid structures, equation of state etc.
Advantages:• Should resolve structure of lower-density gas with
better precision• Shock treatment is effective – hopefully can
estimate shock heating temperature.Disadvantages:• Uniform grid wastes memory on vacuum -> use
Adaptive Mesh refinement• Can present grid artifacts
Using Helmholtz EOS – more complex than Γ/ideal-gas𝐹 = 𝑈 − 𝑇𝑆
9-species nuclear abundance network1H 3He 4He12C14N16O20Ne24Mg56Ni
Multipole gravity solver
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Simulation
• Code written for FLASH 3 – 3D, metal tracing, particle simulation
• Current version for FLASH 4.6 – 2D cylindrical
• Aims:• Import new companion star models from MESA
• Edit code to allow for new supernova explosion models e.g. W7 with updated abundances, N100 so far.
• Adapt FLASH 3 code improvements to newer version – allows us to look at flows more accurately, capture of material.
• Export surviving companion model for long-term evolution – MESA
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Resolution: 11 levels of refinement around star+SN9 elsewhere
~15-18,000 blocks of 8x8 grid cells.
Companion star model is late main-sequence, 1.16 M⊙.
Preliminary results – W7
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Resolution:10 levels of refinement around star+SN8 elsewhere
12-14,000 blocks of 8x8 cells.
Companion star model is close to ZAMS.
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Resolution
AMR: x/y
x is max. levels of refinement outside of star regiony is max. levels of refinement inside star region
Pan, Ricker & Taam (2010).
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Resolution issues
Left: resolution 9/11Right: resolution 7/9
Instabilities on small scale might be exaggerated at short timescales – non-spherical shape. Appears to be solved by using shell-based supernova model.
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N100 (1D angle-averaged) with 1.16 M⊙ late MS star. P= 1.18 days.
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Left: main sequence ‘B’ (Pan et al. ApJ 2012)Right: late main sequence, sub-solar mass ‘model 3’
N100 companion comparison
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Main parameters to retrieve:
Elemental distribution – want to perform long-term evolution simulation of the companion (e.g. 56Ni)
Shock heating – want to estimate luminosity of SN to match with observations
Ejecta cavity angle – important implications in SNR shape.
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Future plans
• Simulate WD during companion star relaxation – inspect effects of Roche-lobe shape.
• Move to a 3D simulation – more accurate depiction of ejecta asymmetry, instabilities (mixing?)
• Include rotation and orbital motion – better estimates for companion kick velocity
• Radiative transfer calculations in FLASH – RadTrans module available in version 4.
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Thank you for listening!