Astrophys. J., 857, 111-111 (2018/April-3)
Stellar yields of rotating first stars. II. Pair-instability supernovae and comparison with observations.
TAKAHASHI K., YOSHIDA T. and UMEDA H.
Abstract (from CDS):
Recent theory predicts that first stars are born with a massive initial mass of >=100 M☉. Pair-instability supernova (PISN) is a common fate for such massive stars. Our final goal is to prove the existence of PISNe and thus the high-mass nature of the initial mass function in the early universe by conducting abundance profiling, in which properties of a hypothetical first star is constrained by metal-poor star abundances. In order to determine reliable and useful abundances, we investigate the PISN nucleosynthesis taking both rotating and nonrotating progenitors for the first time. We show that the initial and CO core mass ranges for PISNe depend on the envelope structures: nonmagnetic rotating models developing inflated envelopes have a lower shifted CO mass range of ∼70-125 M☉, while nonrotating and magnetic rotating models with deflated envelopes have a range of ∼80-135 M☉. However, we find no significant difference in explosive yields from rotating and nonrotating progenitors, except for large nitrogen production in nonmagnetic rotating models. Furthermore, we conduct the first systematic comparison between theoretical yields and a large sample of metal-poor star abundances. We find that the predicted low [Na/Mg] ∼ -1.5 and high [Ca/Mg] ∼0.5-1.3 abundance ratios are the most important to discriminate PISN signatures from normal metal-poor star abundances, and confirm that no currently observed metal-poor star matches with the PISN abundance. An extensive discussion on the nondetection is presented.
© 2018. The American Astronomical Society. All rights reserved.
nuclear reactions, nucleosynthesis, abundances - stars: abundances - stars: Population III - stars: rotation
VizieR on-line data:
<Available at CDS (J/ApJ/857/111): table2.dat table5.dat mr160.dat mr180.dat mr200.dat mr220.dat mr240.dat mr260.dat nr180.dat nr200.dat nr220.dat nr240.dat nr260.dat nr280.dat nm160.dat nm180.dat nm200.dat nm220.dat nm240.dat nm260.dat>
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