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
Dynamics of Type-II 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
Hydrodynamical simulations of type-II supernovae in one and two dimensions are performed for the revival phase of the delayed shock by neutrino energy deposition. Starting with a postcollapse model of the 1.31 M⊙ iron core of a 15 M⊙ star immediately after the stagnation of the prompt shock about 10 ms after core bounce, the models are followed for several hundred milliseconds with varied neutrino fluxes from the neutrino sphere. The variation of the neutrino luminosities is motivated by the considerable increase of the neutrino emission due to convective processes inside and close to the neutrino sphere (see Janka 1993), which are driven by negative gradients of entropy and electron concentration left behind by the prompt shock (Burrows & Fryxell 1992, Janka & Müller 1992). The size of this luminosity increase remains to be quantitatively analyzed yet and may require multi-dimensional neutrino transport. However, in the presented simulations the region below the neutrino sphere is cut out and replaced by an inner boundary condition, so that the convective zone is only partially included and the neutrino flows are treated as a freely changeable energy source.
For small neutrino luminosities the energy transfer to the matter is insufficient to revive the stalled shock. However, there is a sharp transition to successful explosions, when the neutrino luminosities lie above some ‘threshold value’. Once the shock is driven out and the density and temperature of the matter between neutrino sphere and shock start to decrease during the expansion, suitable conditions for further neutrino energy deposition are maintained, and an explosion results.
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- Supernovae and Supernova RemnantsIAU Colloquium 145, pp. 109 - 118Publisher: Cambridge University PressPrint publication year: 1996
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