Abstract
In this chapter outlines some of the consequences of supernova explosions for related areas of astrophysics. Topics include the formation of neutron stars and black holes, the postsupernova nature of former binary companion stars, emission of neutrinos and gravitational waves, supernova nucleosynthesis, injection of dust grains into the interstellar medium, effects of the injection of energy and momentum (feedback) on the surroundings and host galaxies of supernovae, the chemical evolution of the Universe, cosmic-ray production, gamma-ray emission, effects of relatively nearby supernovae on the solar system, and the possible effects of nearby supernovae on life.
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- 1.
Several objects with magnetic fields ∼ 1013 G are thought to be relatively old ( ∼ 105 to 106 years) “fossil” magnetars (Rea et al. 2013).
- 2.
- 3.
- 4.
During their late, precollapse, neutrino-cooling phases of evolution, massive (\(\gtrsim 20\) M⊙) stars emit neutrinos at MeV energies. The flux is low compared to that from a core-collapse, but future detection of such neutrinos from a nearby massive star such as Betelgeuse could provide a much earlier alert, hours, days, or even months before collapse (Kato et al. 2015; Patton et al. 2017; Asakura et al. 2016).
- 5.
Also known as the p-process.
- 6.
As opposed to the proton-rich neutrino-driven wind mentioned above for the νp-process; both could occur in nature, e.g., an evolving neutrino-driven wind could be neutron-rich and proton-rich at different times.
- 7.
- 8.
If, however, star formation extended down to 0.8 M⊙, some observed low-metallicity stars could be “Population III survivors” that have accreted metals from the ISM (Komiya et al. 2010).
- 9.
[Fe∕H] ≡ log(Fe∕H) star − log(Fe∕H) Sun , where Fe∕H is the iron-to hydrogen abundance ratio. Thus, for example, in a star of [Fe∕H] = −6, the Fe∕H ratio is 106 times lower than it is in the Sun.
- 10.
Most very metal-deficient stars are carbon-enhanced (CEMP stars: carbon-enhanced metal-poor stars). Some CEMP stars also have high abundances of s-process elements; many of these stars are known to be in binaries, and they are thought to have acquired their carbon and s-process elements by accretion from a companion AGB star rather than from a supernova (Bonifacio et al. 2015).
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Branch, D., Wheeler, J.C. (2017). Consequences of Supernovae. In: Supernova Explosions. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-55054-0_24
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