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The fate of electron-capture supernovae in binaries
Savvas Chanlaridis, Götz Gräfener, Norbert Langer
John Antoniadis
credit: WISE
Savvas Chanlaridis, Götz Gräfener, Norbert Langer
John Antoniadis
credit: WISE
The fate of electron-capture supernovae in binaries John Antoniadis - - PowerPoint PPT Presentation
The fate of electron-capture supernovae in binaries John Antoniadis - - PowerPoint PPT Presentation
14 th Bonn NS workshop 17 February 2020 The fate of electron-capture supernovae in binaries John Antoniadis Savvas Chanlaridis , Gtz Grfener, Norbert Langer ArXiv: 1912.07608 credit: WISE 14 th Bonn NS workshop 17 February 2020 Type
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Electron-capture supernovae (ECSNe): a primer
What about stars in between? A difficult question…
ZAMS masses below ~7 Msun make CO white dwarfs ZAMS masses above ~10 Msun make neutron stars / black holes
Dohertly et al. 2015
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Electron-capture supernovae (ECSNe): a primer 7—10 Msun mass range is dominated by super-AGB stars: non-explosive carbon burning
Thermal pulses Second dredge-up
- ff-centre C-burning
weak interactions
Poelarends et al. 2008 Poelarends et al. 2008 Farmer et al. 2015 Schwab et al. 2017
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Electron-capture supernovae (ECSNe): a primer Neon consumes a lot of electrons leading to collapse electron consumption vs runaway nuclear burning Outcome depends sensitively on initial conditions (density) and flame propagation core-collapse ECSN thermonuclear ECSN multi-D simulations for 𝜍!
≃ 10"#gcm$ predict tECSNe that
eject 0.1–1.0 Msun and leave behind small bound ONeFe white dwarfs (Jones et al. 2016/2019).
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ECSNe in binaries In isolation, very few SAGB stars reach 𝑁%& What about binaries? Some aspects more complicated, but if the H-envelope is removed then 2DU and thermal pulses are avoided! More (all?) SAGB stars reach 𝑁%& Core grows via stable shell burning
Dohertly et al. 2015
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2.5 Msun helium star, solar metallicity
JA, Chanlaridis, Gräfener & Langer, 2020, A&A; ArXiv:1912.07608
ECSNe in binaries
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ECSNe in binaries
JA, Chanlaridis, Gräfener & Langer, 2020, A&A; ArXiv:1912.07608
carbon burning helium burning
- xygen ignition
shells merge
2.5 Msun helium star, solar metallicity
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ECSNe in binaries
JA, Chanlaridis, Gräfener & Langer, 2020, A&A; ArXiv:1912.07608
2.5 Msun helium star, solar metallicity
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ECSNe in binaries What flavour of Type Ia? ✓Short delay times in respect to star formation ✓Owing to IMF, rates comparable to Ib/c ✓Explosions possible for both stars in a binary
JA, Chanlaridis, Gräfener & Langer, 2020, A&A; ArXiv:1912.07608
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ECSNe in binaries What flavour of Type Ia? ✓The available nuclear energy suffices to unbind the star and to produce ejecta with kinetic energies of order 0.8-1.2 x 1051 erg ✓Short delay times in respect to star formation ✓Owing to IMF, rates comparable to Ib/c ✓Depending on deflagration-to-detonation transition anything from Type Iax to SC Ia is possible ✓Explosions possible for both stars in a binary
JA, Chanlaridis, Gräfener & Langer, 2020, A&A; ArXiv:1912.07608
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