How Massive Single Stars End Their Life

Heger, Alexander; Fryer, Chris L.; Woosley, S. E.; Langer, N.; Hartmann, D. H.

doi:10.1086/375341

Cited by 2,062 publications

(2,408 citation statements)

References 86 publications

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“…Let us suppose, as argued by Heger et al (2003) which are poorly understood, and estimated to occur in ~1-10% of the massive corecollapse events (Fryer et al 2006). To the extent that this is a correct picture we see that a substantial fraction of core-collapse events during the WR epoch will not eject large amounts of newly synthesized material, including 59 Ni, into the superbubble.…”

Section: Discussionmentioning

confidence: 93%

OB Associations, Wolf–Rayet Stars, and the Origin of Galactic Cosmic Rays

Binns

Wiedenbeck

Arnould³

et al. 2007

The Composition of Matter

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Abstract. We have measured the isotopic abundances of neon and a number of other species in the galactic cosmic rays (GCRs) using the Cosmic Ray Isotope Spectrometer (CRIS) aboard the ACE spacecraft. Our data are compared to recent results from two-component (Wolf-Rayet material plus solar-like mixtures) Wolf-Rayet (WR) models. The three largest deviations of galactic cosmic ray isotope ratios from solar-system ratios predicted by these models, 12 C/ 16 O, 22 Ne/ 20 Ne, and 58 Fe/ 56 Fe, are very close to those observed. All of the isotopic ratios that we have measured are consistent with a GCR source consisting of ~20% of WR material mixed with ~80% material with solar-system composition. Since WR stars are evolutionary products of OB stars, and most OB stars exist in OB associations that form superbubbles, the good agreement of our data with WR models suggests that OB associations within superbubbles are the likely source of at least a substantial fraction of GCRs. In previous work it has been shown that the primary 59 Ni (which decays only by electron-capture) in GCRs has decayed, indicating a time interval between nucleosynthesis and acceleration of >10 5 yr. It has been suggested that in the OB association environment, ejecta from supernovae might be accelerated by the high velocity WR winds on a time scale that is short compared to the half-life of 59 Ni. Thus the 59 Ni might not have time to decay and this would cast doubt upon the OB association origin of cosmic rays. In this paper we suggest a scenario that should allow much of the 59 Ni to decay in the OB association environment and conclude that the hypothesis of the OB association origin of cosmic rays appears to be viable.

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Section: Discussionmentioning

confidence: 93%

OB Associations, Wolf–Rayet Stars, and the Origin of Galactic Cosmic Rays

Binns

Wiedenbeck

Arnould³

et al. 2007

The Composition of Matter

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“…5 Theoretical models (see e.g., Heger et al 2003) indicate that the core collapses of main sequence stars with different initial masses and metallicity could result in black holes or neutron stars. The low explosion energy and less mass ejected by SN 2006aj are consistent with a low mass ∼ 20M main sequence star, which is predicted to result in a neutron star after core collapse.…”

Section: Introductionmentioning

confidence: 99%

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Wang

Liu

et al. 2017

ApJ

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Broad-lined type Ic supernovae (SNe Ic-BL) are peculiar stellar explosions that distinguish themselves from ordinary SNe. Some SNe Ic-BL are associated with long-duration ( 2 s) gamma-ray bursts (GRBs). Black holes and magnetars are two types of compact objects that are hypothesized to be central engines of GRBs. In spite of decades of investigations, no direct evidence for the formation of black holes or magnetars has been found for GRBs so far. Here we report the finding that the early peak (t 50 days) and late-time (t 300 days) slow decay displayed in the light curves of both SNe 1998bw (associated with GRB 980425) and 2002ap (not GRB-associated) can be attributed to magnetar spin-down with initial rotation period P 0 ∼ 20 ms, while the intermediate-time (50 t 300 days) exponential decline is caused by radioactive decay of 56 Ni. The connection between the early peak and late-time slow decline in the light curves is unexpected in alternative models. We thus suggest that GRB 980425 and SN 2002ap were powered by magnetars.

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“…The result is that mass loss increases rapidly with mass, so stars with initial mass ∼ 9 M end their lives with most of their H envelopes, while massive stars lose their H envelope by the time of the explosion. The transition to the loss of H envelope occurs at an initial mass ∼ 30 M (Heger et al 2003). Among the massive stars, at low metallicity there is also a transition to the point where the core becomes so massive that there is direct collapse to a black hole without an explosion, ∼ 40 M .…”

Section: Expectations From Massive Star Evolutionmentioning

confidence: 99%

“…Chevalier In going to low metallicity, the mass loss rates due to stellar winds are generally taken to have a dependence ∝ Z n with n ≈ 0.5 (e.g., Heger et al 2003). For O stars and Wolf-Rayet stars there is some observational support for this dependence, but for red supergiants this is simply an estimate.…”

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confidence: 99%

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Supernovae and their Evolution in a Low Metallicity ISM

Chevalier

2008

Proc. IAU

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Abstract.Observations of core collapse supernovae and their progenitors generally support expectations of increasing mass loss with increasing initial mass. Mass loss rates are expected to decline at lower metallicity, and there are prospects for directly testing this for the red supergiant progenitors of Type IIP supernovae. However, there are indications that mass loss rates for high mass early type stars may be overestimated and that there are mass loss mechanisms that do not decline at lower metallicity. In this case, there may be supernova emission from strong circumstellar interaction even at low metallicity. Although there is evidence for dust formation in freely expanding ejecta of supernovae, the quantities are relatively small. Another promising site of dust formation is the circumstellar interaction region, but this should occur in only a fraction of supernovae.

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How Massive Single Stars End Their Life

Cited by 2,062 publications

References 86 publications

OB Associations, Wolf–Rayet Stars, and the Origin of Galactic Cosmic Rays

OB Associations, Wolf–Rayet Stars, and the Origin of Galactic Cosmic Rays

Evidence for Magnetar Formation in Broad-lined Type Ic Supernovae1998bw and 2002ap

Supernovae and their Evolution in a Low Metallicity ISM

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