Book contents
- Frontmatter
- Contents
- Part I Introduction
- Part II Supernovae: Observations Today
- Part III Theory of Thermonuclear Supernovae
- 10 Semi-Steady burning evolutionary sequences for CAL 83 and CAL 87: Super Soft X-ray binaries are supernova Ia progenitors
- 11 Type Ia progenitors: effects of spin-up of white dwarfs
- 12 Terrestrial combustion: feedback to the stars
- 13 Non-spherical delayed detonations
- 14 Numerical simulations of Type Ia supernovae: deflagrations and detonations
- 15 Type Ia supernovae: spectroscopic surprises
- 16 Aspherity effects in supernovae
- 17 Broad lightcurve SNe Ia: asymmetry or something else?
- 18 Synthetic spectrum methods for three-dimensional supernova models
- 19 A hole in Ia? Spectroscopic and polarimetric signatures of SN Ia asymmetry due to a companion star
- 20 Hunting for the signatures of 3-D explosions with 1-D synthetic spectra
- 21 On variations in the peak luminosities of Type Ia supernovae
- Part IV Theory of Core Collapse Supernovae
- Part V Magnetars, N-Stars, Pulsars
- Part VI Gamma-ray Bursts
- Part VII Conference Summary
- References
11 - Type Ia progenitors: effects of spin-up of white dwarfs
Published online by Cambridge University Press: 11 August 2009
- Frontmatter
- Contents
- Part I Introduction
- Part II Supernovae: Observations Today
- Part III Theory of Thermonuclear Supernovae
- 10 Semi-Steady burning evolutionary sequences for CAL 83 and CAL 87: Super Soft X-ray binaries are supernova Ia progenitors
- 11 Type Ia progenitors: effects of spin-up of white dwarfs
- 12 Terrestrial combustion: feedback to the stars
- 13 Non-spherical delayed detonations
- 14 Numerical simulations of Type Ia supernovae: deflagrations and detonations
- 15 Type Ia supernovae: spectroscopic surprises
- 16 Aspherity effects in supernovae
- 17 Broad lightcurve SNe Ia: asymmetry or something else?
- 18 Synthetic spectrum methods for three-dimensional supernova models
- 19 A hole in Ia? Spectroscopic and polarimetric signatures of SN Ia asymmetry due to a companion star
- 20 Hunting for the signatures of 3-D explosions with 1-D synthetic spectra
- 21 On variations in the peak luminosities of Type Ia supernovae
- Part IV Theory of Core Collapse Supernovae
- Part V Magnetars, N-Stars, Pulsars
- Part VI Gamma-ray Bursts
- Part VII Conference Summary
- References
Summary
Abstract
The effects of rotation in progenitor models for Type Ia supernovae are addressed. After discussing processes of angular momentum transport in carbon+oxygen white dwarfs, we investigate pre-explosion conditions of accreting white dwarfs. It is shown that differential rotation will persist throughout the mass accretion phase, with a shear strength near the threshold value for the dynamical shear instability. It is also found that rotational effects stabilise the helium shell source and reduce the carbon abundance in the accreted envelope.
Introduction
Unlike core collapse supernovae, Type Ia supernovae (SNe Ia) occur exclusively in binary systems (e.g. Livio 2000). Although it is still unclear which kinds of binary systems lead to SNe Ia, non-degenerate stars such as main sequence stars, red giants or helium stars are often assumed as the white dwarf companion (e.g. Hachisu et al. 1999, Langer et al. 2000, Han & Podsiadlowski 2003, Yoon & Langer 2003). This leads us to consider the spin-up of the white dwarf, since the transfered matter from those companions should form a Keplerian disk that carries a large amount of angular momentum. The observation that white dwarfs in cataclysmic variables rotate much faster than isolated ones (Sion 1999) provides evidence that accreting white dwarfs are indeed spun up. A rapidly rotating progenitor may also explain the asphericity implied by the polarizations observed in SNe Ia explosions (Wang, this volume). Here we discuss implications of the spin-up of accreting white dwarfs for the progenitors of SNe Ia.
- Type
- Chapter
- Information
- Cosmic Explosions in Three DimensionsAsymmetries in Supernovae and Gamma-Ray Bursts, pp. 94 - 99Publisher: Cambridge University PressPrint publication year: 2004
References
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