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The Progenitor-Remnant Connection of Neutrino-Driven Supernovae Across the Stellar Mass Range

Published online by Cambridge University Press:  28 July 2017

Thomas Ertl
Thomas Ertl*
Affiliation:
Max-Planck-Institut für Astrophysik, Postfach 1317, D-85741 Garching, Germany email: tertl@mpa-garching.mpg.de
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Abstract

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We perform hydrodynamic supernova (SN) simulations in spherical symmetry for progenitor models with solar metallicity across the stellar mass range from 9.0 to 120 M⊙ to explore the progenitor-explosion and progenitor-remnant connections based on the neutrino-driven mechanism. We use an approximative treatment of neutrino transport and replace the high-density interior of the neutron star (NS) by an inner boundary condition based on an analytic proto-NS core-cooling model, whose free parameters are chosen to reproduce the observables of SN 1987A and the Crab SN for theoretical models of their progenitor stars.

Judging the fate of a massive star, either a neutron star (NS) or a black hole (BH), solely by its structure prior to collapse has been ambiguous. Our work and previous attempts find a non-monotonic variation of successful and failed supernovae with zero-age main-sequence mass. We identify two parameters based on the “critical luminosity” concept for neutrino-driven explosions, which in combination allows for a clear separation of exploding and non-exploding cases.

Continuing our simulations beyond shock break-out, we are able to determine nucleosynthesis, light curves, explosion energies, and remnant masses. The resulting NS initial mass function has a mean gravitational mass near 1.4 M⊙. The average BH mass is about 9 M⊙ if only the helium core implodes, and 14 M⊙ if the entire pre-SN star collapses. Only ~10% of SNe come from stars over 20 M⊙, and some of these are Type Ib or Ic.

Keywords

nuclear reactionsnucleosynthesisabundancesstars: black holesstars: massivestars: neutronsupernovae: generalhydrodynamicsneutrinos
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 74 - 77
Copyright
Copyright © International Astronomical Union 2017 

References

Burrows, A. & Goshy, J., 1993, ApJ (Letters), 416, L75 Google Scholar
Ertl, T., Janka, H.-T., Woosley, S. E., Sukhbold, T., & Ugliano, M., 2016, ApJ, 818, 124 Google Scholar
Özel, F. & Freire, P., 2016, ARA&A, 54, 401 Google Scholar
Lentz, E. J., Bruenn, S. W., Hix, W. R., et al. 2015, ApJ (Letters), 807, L31 Google Scholar
Lodders, K., 2003, ApJ, 591, 1220 Google Scholar
Melson, T., Janka, H.-T., & Marek, A., 2015, ApJ (Letters), 801, L24 Google Scholar
Melson, T., Janka, H.-T., Bollig, R., et al. 2015, ApJ (Letters), 808, L42 CrossRefGoogle Scholar
Smartt, S. J., 2015, PASA, 32, e016 Google Scholar
Sukhbold, T., Ertl, T., Woosley, S. E., Brown, J. M., & Janka, H.-T., 2016, ApJ, 821, 38 CrossRefGoogle Scholar
Ugliano, M., Janka, H.-T., Marek, A., & Arcones, A., 2012, ApJ, 757, 69 Google Scholar