Vertical Shear-Wave Velocity Profiles Generated from Spectral
Lessons from Spectral Evolution and High-Velocity Features in Core-Normal Type Ia
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Transcript of Lessons from Spectral Evolution and High-Velocity Features in Core-Normal Type Ia
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Lessons from Spectral Evolution and
High-Velocity Features in
Core-Normal Type Ia
J. Craig WheelerOn Behalf of the Austin Mafia:
Howie Marion (+CfA), Jozsef Vinko (+ U. of Szeged), Jeff Silverman (+ UCB), Robert Quimby (+IPMU)
Texas A&M, April 9, 2103
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Outline
I. Spectral Evolution – Deflagration to Detonation Models
II. => Single Degenerate?
III. High-Velocity Features (as opposed to High Velocity SN Ia)
IV. Collision with a CSM?
I. Conclusions
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Typical Def/Det Composition Structure (Höflich et al. 2004)
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My conviction: 1D deflagration to detonation models do a pretty good job of accounting for the multi-band light curves and spectral evolution of Core Normal SN Ia
Wheeler et al. (1998)
Blondin et al. (2013)
Optical, UV, NIR spectra
Pre-maximum to nebular
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With some perturbation, off-center def/det transition, can account for polarization (Höflich et al. 2006)
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Deflagration/Detonation models do a pretty good job of accounting for the spectral evolution.
Still uncertain physics of deflagration to detonation transition, but see recent work of Poludnenko et al. Paradigm shift through highly-resolved direct numerical simulations of turbulent combustion in hydrogen flames: no distributed flame.
1D Def/Det models are not the last word, but they set the bar: any competing model must do at least as good; not just light curves, but spectral evolution.
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Röpke et al. (2012)
“Hard collision” of two white dwarfs, detonation.Issues with initiating, propagating detonation with level set methodLikely problems with polarization, nebular line profiles
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Seitenzahl et al. (2103) – parametrized 3D Det/Def models, a challenge for the future.
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Does the relative success of Def/Det models imply single degenerate progenitors?
Def/Det models seem to demand a relatively slow evolution to central carbon ignition in a carbon/oxygen white dwarf very near the Chandrasekhar mass, runaway to form deflagration, transition to detonation.
Consistent with classic models of single-degenerate evolution.
But
Relatively slow double-degenerate disruption (10s of orbits??) might do the job (Dan et al. 2011, 2012; but see Kasen talk).
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High-Velocity Features
Seen prominently in Ca NIR triplet prior to maximum, but also in Ca H&K. Si II, other lines.
Clue to burning or to CSM?
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Gerardy et al. (2004)
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Quimby et al. (2006)
“Linear” blue wing in Si II
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High velocity Ca II NIR triplet + OI? (Marion, Vinko, JCW)
Must observe well before maximum, early detection critical.
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SN 2009ig beginning at -14 d (Marion et al. 2013)
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Evolution of Si II (Marion et al. 2013)
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High velocity and photospheric components of Si II, Si III, S II, Fe II (Marion et al. 2013).
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Marion HET snapshot data
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Evolution of High-Velocity Features and Photospheric Features (Marion et al. 2013).6000 km/s
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Silverman – BSNIP data Ca NIR
HVF exist in all subtypes (core normal. 91bg, 91T), both high velocity and normal velocity in X. Wang classification scheme.
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The high-velocity Si II blue wing extends up to the blue absorption of the Ca II NIR that extends to >30,000 km/s in blue wing (Quimby, et al. 2006)
High velocity Si II must come from the white dwarf
High velocity Ca from the CSM??
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Chevalier – forward, reverse shocks, RT unstable contact discontinuity
H, He, primordial Ca
Contact Discontinuity
Si, IME
H, He, primordial Ca
Si, IME
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Gerardy et al. (2004)
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Gerardy et al. (2004)
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Spectropolarimetry of Core Normal Type Ia SN2001el (Wang et al. 2001)
Ca II NIR High-Velocity feature is significantly polarized
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HVF Conclusions
High-velocity features are common before maximum, but not universal (~90% ??; Silverman examining BSNIP data).
High-velocity features are distinctly separate from the photosphere by ~ 6000 km/s, kinematically detached.
High-velocity features are polarized.
Highest velocity HV Si ~ lowest velocity HV Ca.
Impact of SN ejecta on CSM shell, m ~ few hundredths of Msun, with primordial Ca gives a reasonable representation of the HVfeatures.
If CSM shell, must lie at << 1015 cm to avoid contamination of early light curve, must have large covering factor to be so common, but sufficiently asymmetric to account for polarization.
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Conclusions
Deflagration to Detonation models work well for spectral evolution of Core Normal SN Ia (and some sub-varieties).
Consistent with, but does not demand single degenerate evolution
High-velocity features are strongly suggestive of a circumstellar structure of small mass (~ few 0.01 Msun) and radius (typical size of orbit, ~ 1012 cm, would probably be adequate).
Ca could be primordial, but do not know major constituent of CSM, H? He? C? O?
SD?? DD??
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Credit: David A. Hardy
Type Ia