On the mass of supernova progenitors: the role of the $^{12}$C$+^{12}$C reaction. (arXiv:1901.00173v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Straniero_O/0/1/0/all/0/1">Oscar Straniero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Piersanti_L/0/1/0/all/0/1">Luciano Piersanti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dominguez_I/0/1/0/all/0/1">Inmaculata Dominguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tumino_A/0/1/0/all/0/1">Aurora Tumino</a>
A precise knowledge of the masses of supernova progenitors is essential to
answer various questions of modern astrophysics, such as those related to the
dynamical and chemical evolution of Galaxies. In this paper we revise the upper
bound for the mass of the progenitors of CO white dwarfs (mup) and the lower
bound for the mass of the progenitors of normal type II supernovae (mups). In
particular, we present new stellar models with mass between 7 and 10 msun,
discussing their final destiny and the impact of recent improvements in our
understanding of the low energy rate of the c12c12 reaction.
A precise knowledge of the masses of supernova progenitors is essential to
answer various questions of modern astrophysics, such as those related to the
dynamical and chemical evolution of Galaxies. In this paper we revise the upper
bound for the mass of the progenitors of CO white dwarfs (mup) and the lower
bound for the mass of the progenitors of normal type II supernovae (mups). In
particular, we present new stellar models with mass between 7 and 10 msun,
discussing their final destiny and the impact of recent improvements in our
understanding of the low energy rate of the c12c12 reaction.
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