The Supernova Channel of Super‐AGB Stars

Poelarends, A.J.T.; Herwig, Falk; Langer, N.; Heger, Alexander

doi:10.1086/520872

Cited by 318 publications

(462 citation statements)

References 61 publications

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“…A recent comparison between the inferred properties of massive O and B stars within 500 pc (Hohle et al 2010) using three modern evolution codes (Schaller et al 1992;Bertelli et al 1994;Claret 2004) indicate uncertainties at the ∼20 -25 % level. Similar degrees of uncertainty were found when computing the mass limits associated with O-Ne-Mg core formation in intermediate mass stars (Poelarends et al 2008).…”

Section: The Current Framework For Computing Evolutionsupporting

confidence: 68%

Presupernova structure of massive stars

Sukhbold

Arnett

2011

Astrophys Space Sci

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Issues concerning the structure and evolution of core collapse progenitor stars are discussed with an emphasis on interior evolution. We describe a program designed to investigate the transport and mixing processes associated with stellar turbulence, arguably the greatest source of uncertainty in progenitor structure, besides mass loss, at the time of core collapse. An effort to use precision observations of stellar parameters to constrain theoretical modeling is also described.

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Section: The Current Framework For Computing Evolutionsupporting

confidence: 68%

Presupernova structure of massive stars

Sukhbold

Arnett

2011

Astrophys Space Sci

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“…In the following I summarize the main results of self-consistent fully evolutionary studies of these stars. However, for the sake of conciseness only a brief overview of the very interesting physical phenomena occurring during the carbon burning phase in this mass interval will be given, and I refer 54 E. García-Berro the interested reader to the series of papers by Ritossa et al (1996), García-Berro et al (1997), Iben et al (1997), Ritossa et al (1999), the more recent studies of Siess (2006Siess ( , 2007Siess ( , 2009Siess ( , 2010 which confirm the main findings of the previous papers, and Poelarends et al (2008). Also, the possible outcomes of the evolution of SAGB stars will be analyzed, but I will not discuss here other interesting aspects, like the possible contribution of this range of masses to r-process nucleosynthesis (Ning et al 2007, Wanajo et al 2006.…”

Section: The Formation and Evolution Of One White Dwarfssupporting

confidence: 56%

“…This is because the mass-loss rate depends on the metallicity of the envelope, which depends on the prescription adopted for determining the position of the inner edge of the convective envelope (Gil-Pons et al 2005, 2007. However, in contrast to what occurs for normal AGB stars, the number of thermal pulses necessary to remove the massive envelope is in this case very large, ∼10 3 (Poelarends et al 2008). Following the evolution during the thermally pulsing phase is thus a hard task, and we rely on approximations.…”

Section: Possible Outcomes Of Sagb Starsmentioning

confidence: 99%

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The Formation and Evolution of ONe White Dwarfs: Prospects for Accretion Induced Collapse

Garcı́a–Berro

2011

Proc. IAU

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Abstract. I review our current understanding of the evolution of stars which experience carbon burning under conditions of partial electron degeneracy and ultimately become thermally pulsing "super" asymptotic giant branch (SAGB) stars with electron-degenerate cores composed primarily of oxygen and neon. The range in stellar mass over which this occurs is very narrow and the interior evolutionary characteristics vary rapidly over this range. Consequently, while those stars with larger masses (∼11 M ) are likely to undergo electron-capture accretion induced collapse, those models with smaller masses (8.5 < ∼ M/M < ∼ 10.5) will presumably form massive (M > ∼ 1.1 M ) white dwarfs. The final outcome depends sensitively on the adopted mass-loss rates, the chemical composition of the massive envelopes, and on the adopted prescription for convective mixing.

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“…It has previously been demonstrated that the initial mass range for producing EC SNe is smaller in single stars (Poelarends et al 2008) compared to binary stars in non-degenerate systems (Podsiadlowski et al 2004). …”

Section: The Zams Progenitor Masses Of Our Naked Helium Starsmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

415

613

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The explosion of ultra-stripped stars in close binaries can lead to ejecta masses < 0.1 M ⊙ and may explain some of the recent discoveries of weak and fast optical transients. In Tau ris et al. (2013), it was demonstrated that helium star companions to neutron stars (NSs) may experience mass transfer and evolve into naked ∼ 1.5 M ⊙ metal cores, barely above the Chandrasekhar mass limit. Here we elaborate on this work and present a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe). In particular, we examine the binary parameter space leading to electron-capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, and determine the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic. We mainly evolve systems where the SN progenitors are helium star donors of initial mass M He = 2.5 − 3.5 M ⊙ in tight binaries with orbital periods of P orb = 0.06 − 2.0 days, and hosting an accreting NS, but we also discuss the evolution of wider systems and of both more massive and lighter -as well as single -helium stars. In some cases we are able to follow the evolution until the onset of silicon burning, just a few days prior to the SN explosion. We find that ultra-stripped SNe are possible for both EC SNe and Fe CCSNe. EC SNe only occur for M He = 2.60 − 2.95 M ⊙ depending on P orb . The general outcome, however, is an Fe CCSN above this mass interval and an ONeMg or CO white dwarf for smaller masses. For the exploding stars, the amount of helium ejected is correlated with P orb -the tightest systems even having donors being stripped down to envelopes of less than 0.01 M ⊙ . We estimate the rise time of ultra-stripped SNe to be in the range 12 hr − 8 days, and light curve decay times between 1 and 50 days. A number of fitting formulae for our models are provided with applications to population synthesis. Ultrastripped SNe may produce NSs in the mass range 1.10 − 1.80 M ⊙ and are highly relevant for LIGO/VIRGO since most (possibly all) merging double NS systems have evolved through this phase. Finally, we discuss the low-velocity kicks which might be imparted on these resulting NSs at birth.

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The Supernova Channel of Super‐AGB Stars

Cited by 318 publications

References 61 publications

Presupernova structure of massive stars

Presupernova structure of massive stars

The Formation and Evolution of ONe White Dwarfs: Prospects for Accretion Induced Collapse

Ultra-stripped supernovae: progenitors and fate

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