Book contents
- Frontmatter
- Contents
- Participants
- Preface
- Acknowledgements
- Observations of Supernovae and the Cosmic Distance Scale
- Type Ia Supernovae
- Type Ib and Type II Supernovae
- Recent Advances in Supernova Theory
- Dynamics of Type-II Supernovae
- Hydrodynamics and Theoretical Light Curves of SNe II
- Instabilities and Mixing in Type II-P and II-b Supernovae
- Progenitors and Hydrodynamics of Type II and Ib Supernovae
- Statistical Analysis of Supernovae and Progenitors of SN Ib and SN Ic
- Supernova Nucleosynthesis in Massive Stars
- Nuclear Weak Processes in Presupernova Stars
- SN 1987A, SN 1993J, and Other Supernovae
- Supernovae and Circumstellar Matter
- Supernova Remnants
- Catalogues
- List of Contributed Papers
Progenitors and Hydrodynamics of Type II and Ib Supernovae
from Type Ib and Type II Supernovae
Published online by Cambridge University Press: 04 August 2010
- Frontmatter
- Contents
- Participants
- Preface
- Acknowledgements
- Observations of Supernovae and the Cosmic Distance Scale
- Type Ia Supernovae
- Type Ib and Type II Supernovae
- Recent Advances in Supernova Theory
- Dynamics of Type-II Supernovae
- Hydrodynamics and Theoretical Light Curves of SNe II
- Instabilities and Mixing in Type II-P and II-b Supernovae
- Progenitors and Hydrodynamics of Type II and Ib Supernovae
- Statistical Analysis of Supernovae and Progenitors of SN Ib and SN Ic
- Supernova Nucleosynthesis in Massive Stars
- Nuclear Weak Processes in Presupernova Stars
- SN 1987A, SN 1993J, and Other Supernovae
- Supernovae and Circumstellar Matter
- Supernova Remnants
- Catalogues
- List of Contributed Papers
Summary
We review critical physics affecting the observational characteristics of those supernovae that occur in massive stars. Particular emphasis is given to 1) how mass loss, either to a binary companion or by a radiatively driven wind, affects the type and light curve of the supernova, and 2) the interaction of the outgoing supernova shock with regions of increasing ρr3 in the stellar mantle. One conclusion is that Type II-L supernovae may occur in mass exchanging binaries very similar to the one that produced SN 1993J, but with slightly larger initial separations and residual hydrogen envelopes (∼1 M⊙ and radius ∼ several AU). The shock interaction, on the other hand, has important implications for the formation of black holes in explosions that are, near peak light, observationally indistinguishable from ordinary Type II-p and Ib supernovae.
Some Generalities
There is broad agreement regarding the qualitative evolution of single stars sufficiently massive to ignite carbon burning non-degenerately (e.g., Woosley & Weaver 1986; Weaver & Woosley 1993; Nomoto & Hashimoto 1986, 1988). Given the usual, relevant caveats about the treatment of convective mixing, convective overshoot, and semiconvection, it is agreed that stars of approximately 8 to 12 M⊙(±1 M⊙ depending upon initial helium abundance and convective parameters) will not proceed to silicon burning in hydrostatic equilibrium, but will stop prior to central neon ignition and experience a complicated subsequent evolution in which degenerate flashes play an important role.
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- Chapter
- Information
- Supernovae and Supernova RemnantsIAU Colloquium 145, pp. 137 - 148Publisher: Cambridge University PressPrint publication year: 1996