How binarity affects the observed initial and final core masses of hydrogen-rich, Type II supernova progenitors. (arXiv:2002.07230v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zapartas_E/0/1/0/all/0/1">Emmanouil Zapartas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mink_S/0/1/0/all/0/1">Selma E. de Mink</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Justham_S/0/1/0/all/0/1">Stephen Justham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Smith_N/0/1/0/all/0/1">Nathan Smith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Renzo_M/0/1/0/all/0/1">Mathieu Renzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koter_A/0/1/0/all/0/1">Alex de Koter</a>
The majority of massive stars, the progenitors of core-collapse supernovae
(SNe), are found in close binary systems. Zapartas et al. (2019) modeled the
fraction of hydrogen-rich, Type II SN progenitors which have their evolution
affected by mass exchange with their companion, finding this to be between 1/3
and 1/2 for most assumptions. Here we study in more depth the impact of this
binary history of Type II SN progenitors on their final pre-SN core mass
distribution, using population synthesis simulations. We find that binary star
progenitors of Type II SNe typically end their life with a larger core mass
than they would have had if they had lived in isolation, because they gained
mass or merged with a companion before explosion. The combination of the
diverse binary evolutionary paths typically lead to a marginally shallower
final core mass distribution. Discussing our results in the context of the red
supergiant problem, i.e., the reported lack of detected high luminosity
progenitors, we conclude that binary evolution does not seem to significantly
affect the issue. This conclusion is quite robust against our variations in the
assumptions of binary physics. We also predict that inferring the initial
masses of Type II SN progenitors from “age-dating” its surrounding environment
systematically yields lower masses compared to methods that probe the pre-SN
core mass or luminosity. A robust discrepancy between the inferred initial
masses of a SN progenitor from those different techniques could indicate an
evolutionary history of binary mass accretion or merging.
The majority of massive stars, the progenitors of core-collapse supernovae
(SNe), are found in close binary systems. Zapartas et al. (2019) modeled the
fraction of hydrogen-rich, Type II SN progenitors which have their evolution
affected by mass exchange with their companion, finding this to be between 1/3
and 1/2 for most assumptions. Here we study in more depth the impact of this
binary history of Type II SN progenitors on their final pre-SN core mass
distribution, using population synthesis simulations. We find that binary star
progenitors of Type II SNe typically end their life with a larger core mass
than they would have had if they had lived in isolation, because they gained
mass or merged with a companion before explosion. The combination of the
diverse binary evolutionary paths typically lead to a marginally shallower
final core mass distribution. Discussing our results in the context of the red
supergiant problem, i.e., the reported lack of detected high luminosity
progenitors, we conclude that binary evolution does not seem to significantly
affect the issue. This conclusion is quite robust against our variations in the
assumptions of binary physics. We also predict that inferring the initial
masses of Type II SN progenitors from “age-dating” its surrounding environment
systematically yields lower masses compared to methods that probe the pre-SN
core mass or luminosity. A robust discrepancy between the inferred initial
masses of a SN progenitor from those different techniques could indicate an
evolutionary history of binary mass accretion or merging.
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