Abstract
In this chapter discusses various progenitor systems that might lead to the observed phenomena of Type Ia supernovae (SN Ia) and related events. All constraints point to SN Ia arising in carbon-oxygen white dwarfs that accrete mass or merge in binary systems. The canonical competing scenarios for progenitor evolution are those with a white dwarf and a less evolved companion, the single-degenerate proposal, and those with two white dwarfs, the double-degenerate proposal. Binary evolution simulations coupled with population synthesis simulations give constraints on possible progenitors. Single degenerate models must provide just the right rate of mass accretion onto the white dwarf, not too fast and not too slow. The companion star must have sufficient mass to grow the white dwarf with even an inefficient mass-transfer process. The donor stars might be rich in either hydrogen or helium. Among other possible observed progenitor systems are recurrent novae, but establishing a robust connection with known systems has proven difficult. Some models require less than the Chandrasekhar mass by igniting a surface shell of helium that compresses the inner carbon-oxygen core to trigger a detonation. Some double-degenerate models invoke the rapid disruption of one of the white dwarfs or the dynamical collision of two white dwarfs to trigger dynamical carbon burning. The chapter concludes with a discussion of other progenitor constraints: archival observations of explosion sites, statistics of possibly related binary X-ray sources, possible interaction of ejecta with circumstellar matter or a companion star, and the nature of the ultimate supernova remnant.
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Notes
- 1.
An SAGB star with a carbon core surrounded by oxygen and neon might produce a single-star explosion (Denissenkov et al. 2013), but such a configuration is unlikely to resemble a typical SN Ia. For novel speculations concerning explosions of single white dwarfs, see Chiosi et al. (2015), Di Stefano et al. (2015), Graham et al. (2015d), and Bramante (2015).
- 2.
Helium white dwarfs can, however, be produced by binary evolution.
- 3.
The period in days, P, and the separation in units of the solar radius, a, are related by P 2 = 1. 38 × 10−2 a 3∕(M 1 + M 2), where M 1 and M 2 are the masses of the two stars in solar units.
- 4.
For a discussion of observational differences between mass-ratio distributions of close and wide companions, see Gullikson et al. (2016). Note also that there are strong selection effects against low secondary masses. Techniques of aperture-masking interferometry coupled with adaptive optics have the power to reveal low-mass companions (Hinkley et al. 2015).
- 5.
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Branch, D., Wheeler, J.C. (2017). Progenitors. In: Supernova Explosions. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-55054-0_21
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