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Single Vs binary star progenitors of Type Iib Sne
Niharika Sravan, pablo Marchant and vicky kalogera
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time domain big data astronomy and supernovae
Plethora of survey projects culminating with the LSST will transform SN science by providing unprecedented insights into supernova: Progenitors Environments
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Time sensitivity Pre-SN variability Progenitor detection
Late stage massive star evolution Stellar interactions Progenitor detection + Companions Light curve and spectral evolution – early detection important! Progenitor structure CSM interactions Remnants End-products of massive star evolution
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Time sensitivity Reducing detection, classification and analysis overhead Need but lack comprehensive database of models in the relevant parameter space
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A Systematic parameter space study of SN progenitors
My work! Focus: Stripped Envelope Supernovae
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Stripped Envelope (SE) Supernovae
H He Core Type II STRIP! SUPERNOVA H He Core SE SNe (Types IIb,Ib,Ic) Core Core He SUPERNOVA
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Stripped Envelope SupernoVae
Important to understanding: stellar winds close binary interactions in massive star evolution MECHANISMS DOMINATING STRIPPING Single Star Progenitors Stellar Winds Binary Star Progenitors Close Binary Interactions
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Test case: Type IIb SupernoVae
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Type IIb SuperNovae Type II Type IIb SUPERNOVA STRIP! SN 2011dh
He Core Type II 99d STRIP! SUPERNOVA time SN 2011dh 202d H He Type IIb Core SUPERNOVA Jerkstrand et al., 2015
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Overview of Type IIb Sne
Luminosity (L☉) Teff (K) Progenitor Observations Luminosity log10(L/L☉) = 4.72 – 5.4 Effective Temperature log10(Teff/K) = 3.58 – 3.8 Light Curves Hydrogen envelope mass 0.01 – 0.5 M☉ Helium core mass 2 – 6 M☉ Abundant ~ 11-12% a,b of all core-collapse SNe 30-40% a,b of all SE SNe Five with detected progenitors Only stripped envelope SN progenitor with detected binary companion a Li et al, 2011 b Smith et al, 2011 Type IIb
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What are the Progenitors of type IIb Sne?
Parameter search space Single star models*: M/M☉ = 10 – 80 Binary star models*: M1/M☉= 10 – 18 M2/M☉= 6 – M1 log10(Porb /d) = 0.0 – 4.0 Conservative and non-conservative MT *solar metallicity, non-rotating Type IIb
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Physical Constraints to match for explaining Type IIb SN Progenitor observations
Progenitor Properties HYDROGEN ENVELOPE MASS 0.01 – 0.5 M☉ HELIUM CORE MASS 2 – 6 M☉ LUMINOSITY log10(L/L☉) = 4.72 – 5.4 EFFECTIVE TEMPERATURE log10(Teff/K) = 3.58 – 3.8 Type IIb
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Can single stars be type IIb Sn progenitors?
Helium core mass Models Models with residual Hydrogen envelope mass 0.01 – 0.5 M☉ Observations Models Sravan et al., in prep Observations NO Luminosity and Teff Type IIb
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Can binary stars be type IIb Sn progenitors?
Parameter space occupied by binary star models reaching core-collapse with 0.01 – 0.5 M☉ residual Hydrogen envelope Can binary stars be type IIb Sn progenitors? Sravan et al., in prep Type IIb
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Can binary stars be type IIb Sn progenitors?
Helium core mass Models with residual Hydrogen envelope mass 0.01 – 0.5 M☉ Observations Sravan et al., in prep Models Observations Models Luminosity and Teff YES! Type IIb
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Summary We find solar-metallicity, non-rotating single stars cannot be Type IIb progenitors Solar-metallicity, non-rotating binary stars can be Type IIb progenitors These systems have: Mass ratios > 0.6 3.2 < log10(Porb,i) < 3.6 Companion luminosity: 4 < log10(L/L☉)< 4.8 Predicted rate ~ 1% of all CC SNe
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Future Work Complete parameter space:
single star rotating models binary star models Mprim > 20M☉ Study light curves from IIb progenitor models
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Thank you!
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