Single Degenerate Models for Type Ia Supernovae: Progenitor’s Evolution and Nucleosynthesis Yields
We review how the single degenerate models for Type Ia supernovae (SNe Ia) works. In the binary star system of a white dwarf (WD) and its non-degenerate companion star, the WD accretes either hydrogen-rich matter or helium and undergoes hydrogen and helium shell-burning. We summarize how the stability and non-linear behavior of such shell-burning depend on the accretion rate and the WD mass and how the WD blows strong wind. We identify the following evolutionary routes for the accreting WD to trigger a thermonuclear explosion. Typically, the accretion rate is quite high in the early stage and gradually decreases as a result of mass transfer. With decreasing rate, the WD evolves as follows: (1) At a rapid accretion phase, the WD increase its mass by stable H burning and blows a strong wind to keep its moderate radius. The wind is strong enough to strip a part of the companion star’s envelope to control the accretion rate and forms circumstellar matter (CSM). If the WD explodes within CSM, it is observed as an “SN Ia-CSM”. (X-rays emitted by the WD are absorbed by CSM.) (2) If the WD continues to accrete at a lower rate, the wind stops and an SN Ia is triggered under steady-stable H shell-burning, which is observed as a super-soft X-ray source: “SN Ia-SSXS”. (3) If the accretion continues at a still lower rate, H shell-burning becomes unstable and many flashes recur. The WD undergoes recurrent nova (RN) whose mass ejection is smaller than the accreted matter. Then the WD evolves to an “SN Ia-RN”. (4) If the companion is a He star (or a He WD), the accretion of He can trigger He and C double detonations at the sub-Chandrasekhar mass or the WD grows to the Chandrasekhar mass while producing a He-wind: “SN Ia-He CSM”. (5) If the accreting WD rotates quite rapidly, the WD mass can exceed the Chandrasekhar mass of the spherical WD, which delays the trigger of an SN Ia. After angular momentum is lost from the WD, the (super-Chandra) WD contracts to become a delayed SN Ia. The companion star has become a He WD and CSM has disappeared: “SN Ia-He WD”. We update nucleosynthesis yields of the carbon deflagration model W7, delayed detonation model WDD2, and the sub-Chandrasekhar mass model to provide some constraints on the yields (such as Mn) from the comparison with the observations. We note the important metallicity effects on 58Ni and 55Mn.
KeywordsSupernova Progenitor White dwarf Nucleosynthesis
This work has been supported by the World Premier International Research Center Initiative (WPI Initiative), MEXT, Japan, and JSPS KAKENHI Grant Numbers JP26400222, JP16H02168, JP17K05382.
- D. Arnett, Supernovae and Nucleosynthesis (Princeton University Press, Princeton, 1996) Google Scholar
- M. Kato, I. Hachisu, H. Saio, Recurrent novae and long-term evolution of mass-accreting white dwarfs—toward the accurate mass retention efficiency (2017). arXiv:1711.01529
- S.-C. Leung, K. Nomoto, Dependence of nucleosynthesis on Model Parameters of Type Ia supernovae. Astrophys. J. Suppl. Ser. (2017, submitted). arXiv:1710.04254
- M. Livio, The progenitors of Type Ia supernovae, in Type Ia Supernovae, Theory and Cosmology, ed. by J.C. Niemeyer, J.W. Truran (Cambridge University Press, Cambridge, 2000), p. 33 Google Scholar
- K. Nomoto, H. Yamaoka, T. Shigeyama, S. Kumagai, T. Tsujimoto, Type I supernovae and evolution of interacting binaries, in Supernovae, Proc. of Session LIV held in Les Houche 1990, ed. by S. Bludmann et al.. NATO ASI Ser. C (North-Holland, Amsterdam, 1994), p. 199. http://supernova.astron.s.u-tokyo.ac.jp/~nomoto/reference Google Scholar
- K. Nomoto, H. Umeda, C. Kobayashi et al., Type Ia supernova progenitors, environmental effects, and cosmic supernova rates, in Type Ia Supernovae, Theory and Cosmology, ed. by J.C. Niemeyer, J.W. Truran (Cambridge University Press, Cambridge, 2000a), p. 63 Google Scholar
- K. Nomoto, T. Suzuki, J. Deng, T. Uenishi, I. Hachisu, Progenitors of Type Ia supernovae: circumstellar interaction, rotation, and steady hydrogen burning, in Supernovae as Cosmological Lighthouses 1604–2004, ed. by Turatto et al.. ASP Conference Series, vol. 342 (2005), p. 105 Google Scholar
- K. Nomoto, M. Kamiya, N. Nakasato, Type Ia supernova models and progenitor scenarios, in IAU Symposium 281, Binary Paths to Type Ia Supernovae Explosions (Cambridge University Press, Cambridge, 2013a), p. 253 Google Scholar
- K. Nomoto, S.-C. Leung, Thermonuclear explosions of Chandrasekhar mass white dwarfs, in Handbook of Supernovae, vol. 2, ed. by A.W. Alsabti, P. Murdin (Springer) (2017), p. 1275. http://supernova.astron.s.u-tokyo.ac.jp/~nomoto/reference CrossRefGoogle Scholar
- D. Sugimoto, M. Fujimoto, K. Nariai, K. Nomoto, in IAU Colloquium 53, White Dwarfs and Variable Degenerate Stars, ed. by H.M. Van Horn, V. Weidemann (University of Rochester, Rochester, 1979), p. 280 Google Scholar
- Yield Table, http://supernova.astron.s.u-tokyo.ac.jp/~nomoto/yields (2018)