Astrophys. J., Suppl. Ser., 237, 13-13 (2018/July-0)
Presupernova evolution and explosive nucleosynthesis of rotating massive stars in the metallicity range -3 <= [Fe/H] <= 0.
LIMONGI M. and CHIEFFI A.
Abstract (from CDS):
We present a new grid of presupernova models of massive stars extending in mass between 13 and 120 M☉, covering four metallicities (i.e., [Fe/H] = 0, -1, -2, and -3) and three initial rotation velocities (i.e., 0, 150, and 300 km s–1). The explosion has been simulated following three different assumptions in order to show how the yields depend on the remnant mass-initial mass relation. An extended network from H to Bi is fully coupled to the physical evolution of the models. The main results can be summarized as follows. (a) At solar metallicity, the maximum mass exploding as a red supergiant (RSG) is of the order of 17 M☉ in the nonrotating case, with the more massive stars exploding as Wolf-Rayet (WR) stars. All rotating models, conversely, explode as WR stars. (b) The interplay between the core He-burning and the H-burning shell, triggered by the rotation-induced instabilities, drives the synthesis of a large primary amount of all the products of CNO, not just 14N. A fraction of them greatly enriches the radiative part of the He core (and is responsible for the large production of F), and a fraction enters the convective core, leading therefore to an important primary neutron flux able to synthesize heavy nuclei up to Pb. (c) In our scenario, remnant masses of the order of those inferred from the first detections of gravitational waves (GW 150914, GW 151226, GW 170104, GW 170814) are predicted at all metallicities for none or moderate initial rotation velocities.
© 2018. The American Astronomical Society. All rights reserved.
stars: evolution - stars: interiors - stars: massive - stars: rotation - supernovae: general
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<Available at CDS (J/ApJS/237/13): table3.dat table5.dat table6.dat table7.dat table8.dat table9.dat>
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