How Much 56Ni Can Be Produced in Core-Collapse Supernovae? Evolution and Explosions of 30-100 M☉ Stars

By H. Umeda, Ken'ichi Nomoto. 2007

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Motivated by the discovery of extremely bright supernovae SNe 1999as and 2006gy, we have investigated how much 56Ni mass can be synthesized in core-collapse massive supernovae (SNe). We calculate the evolution of several very massive stars with initial masses M ⩽ 100 M☉ from the main sequence to the beginning of the Fe core collapse and simulate their explosions and nucleosynthesis. In order to avoid complications associated with strong mass loss, we consider only metal-poor stars with initial metallicity Z = Z☉/200. However, our results are applicable to higher metallicity models with similar C+O core masses. The C+O core mass for the 100 M☉ model is MCO = 42.6 M☉, and this is the heaviest model in the literature for which Fe-core-collapse SN is explored. The synthesized 56Ni mass increases with the increasing explosion energy and progenitor mass. For the explosion energy of E51 ≡ E/1051 ergs = 30, for example, the 56Ni masses of M(56Ni) = 2.2, 2.3, 5.0, and 6.6 M☉ can be produced for the progenitors with initial masses of 30, 50, 80, and 100 M☉ (or C+O core masses MCO = 11.4, 19.3, 34.0, and 42.6 M☉), respectively. We find that producing M(56Ni) ∼ 4 M☉ as seen in SN 1999as is possible for MCO≳ 34 M☉ and E51≳ 20. Producing M(56Ni) ∼ 13 M☉, as suggested for SN 2006gy, requires a too large explosion energy for MCO≲ 43 M☉, but it may be possible with a reasonable explosion energy if MCO≳ 60 M☉.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/39ccedfb08b4b990873395002b47fb33acfa9398

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Citations in the corpus

Light-curve modelling of superluminous supernova 2006gy: collision between supernova ejecta and a dense circumstellar medium (2012, background): “The large amount of 56Ni is not easily produced even by very high-energy core-collapse SNe (Umeda & Nomoto 2008).”
High luminosity, slow ejecta and persistent carbon lines: SN 2009dc challenges thermonuclear explosion scenarios (2010, background): “Beyond this, Umeda & Nomoto (2008) recently constructed a series of core-collapse models from very massive (20–100 M ) progenitors, assuming little fall-back of synthesized 56Ni on to the newly formed black hole.”
Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “M stars also undergo nuclear instability as a result of Si burning, and they pulsate several times (see Figure 3) (Umeda & Nomoto 2008).”
SUPER-LUMINOUS TYPE Ic SUPERNOVAE: CATCHING A MAGNETAR BY THE TAIL (2013, background): “The first assumption is based on the implausibility of a pure 56Ni ejecta; Umeda & Nomoto (2008) found typical 56Ni masses which are at most 20% of the ejecta, while if the ejecta was comprised of more 56Ni than this, we would expect to see spectra dominated by Fe-group rather than intermediate…”
HIGH-DENSITY CIRCUMSTELLAR INTERACTION IN THE LUMINOUS TYPE IIn SN 2010jl: THE FIRST 1100 DAYS (2013, background): “…of Turku, Väisäläntie 20 FI-21500 Piikkiö, Finland 11 INAF-Osservatorio Astronomico di Padova, Vicolo dellOsservatorio 5, I-35122 Padova, Italy SNe (Umeda & Nomoto 2008), to ongoing shock interactions or shock breakout from an extended progenitor (Falk & Arnett 1977; Grasberg & Nadyozhin…”
Progenitors of Core-Collapse Supernovae (2009, background): “In theory 10-20M⊙ of 56Ni can be produced and ejected (Heger and Woosley 2002) in a pair-instability supernova or ∼5M⊙ in a core-collapse of a massive star (Umeda and Nomoto 2008).”
Pulsational Pair-instability Supernovae (2016, background): “It thus seems unlikely that credible models can produce more than about 4 M of 56Ni without encountering the PPI and shrinking in mass first (though see Umeda & Nomoto 2008).”