Evolution of Progenitors for Electron Capture Supernovae

Takahashi, Koh; Yoshida, Takashi; Umeda, Hideyuki

doi:10.1088/0004-637x/771/1/28

Cited by 90 publications

(157 citation statements)

References 45 publications

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“…For stars which do not ignite oxygen, but for which their ONeMg cores are more massive than 1.37 M⊙, the final fate is an EC SN (Nomoto 1987;Podsiadlowski et al 2004;Takahashi et al 2013). Fig.…”

Section: Evolution Leading To An Electron-capture Snmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

395

611

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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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Section: Evolution Leading To An Electron-capture Snmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

395

611

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“…Tauris et al (2015) adopted M ONe,f = 1.43M⊙ as an approximate upper limit for electron-capture SN. In the case of single star evolution in Takahashi et al (2013), a 10.8 M⊙ model ends its evolution as an electron-capture SN and an 11.0 M⊙ model ignites Ne at an off-center region. Off-center Ne ignition and gradual increase in the central temperature around the central density ρC ∼ 10 9 g cm −3 could be predictions of the Fe core formation and core-collapse SN.…”

Section: Summary and Discussionmentioning

confidence: 99%

“…To make initial conditions for hydrodynamics simulations, we first perform stellar evolutionary simulations of CO cores with masses of 1.45, 1.5, 1.6, 1.8, and 2.0 M⊙ supposing that stellar mass loss has already occurred by their hypothetical companion NSs. By removing stellar envelope, the stellar evolutionary simulations are done with a code described in Umeda et al (2012); Takahashi et al (2013); Yoshida et al (2014). The nuclear reaction network consists of 300 species of nuclei (Takahashi et al 2013;Yoshida et al 2014).…”

Section: Stellar Evolution and Progenitor Structuresmentioning

confidence: 99%

“…By removing stellar envelope, the stellar evolutionary simulations are done with a code described in Umeda et al (2012); Takahashi et al (2013); Yoshida et al (2014). The nuclear reaction network consists of 300 species of nuclei (Takahashi et al 2013;Yoshida et al 2014). Schwarzschild criterion is employed as the convection criterion and the convective mixing of the chemical composition is evolved using diffusion equation.…”

Section: Stellar Evolution and Progenitor Structuresmentioning

confidence: 99%

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Neutrino-driven explosions of ultra-stripped Type Ic supernovae generating binary neutron stars

Suwa

Yoshida

Shibata

et al. 2015

Mon. Not. R. Astron. Soc.

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101

116

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We study explosion characteristics of ultra-stripped supernovae (SNe), which are candidates of SNe generating binary neutron stars (NSs). As a first step, we perform stellar evolutionary simulations of bare carbon-oxygen cores of mass from 1.45 to 2.0 M ⊙ until the iron cores become unstable and start collapsing. We then perform axisymmetric hydrodynamics simulations with spectral neutrino transport using these stellar evolution outcomes as initial conditions. All models exhibit successful explosions driven by neutrino heating. The diagnostic explosion energy, ejecta mass, Ni mass, and NS mass are typically ∼ 10 50 erg, ∼ 0.1M ⊙ , ∼ 0.01M ⊙ , and ≈ 1.3M ⊙ , which are compatible with observations of rapidly-evolving and luminous transient such as SN 2005ek. We also find that the ultra-stripped SN is a candidate for producing the secondary low-mass NS in the observed compact binary NSs like PSR J0737-3039.

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“…In particular, we used a mixing length parameter of 2 with a semiconvection efficiency parameter of 1. As the core mass is rather small, weak reactions play an important role in the evolution of the core approaching collapse (e.g., Takahashi, Yoshida, & Umeda 2013;Jones et al 2013;Schwab, Quataert, & Bildsten 2015). Therefore we used the large nuclear network ''mesa151.net'' provided in MESA, which includes 151 nuclei up to 65 Ni with important weak reactions such as electron capture by 33 S and 35 Cl.…”

Section: Progenitormentioning

confidence: 99%

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya

Mazzali

Tominaga

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

105

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We investigate light-curve and spectral properties of ultra-stripped core-collapse supernovae. Ultra-stripped supernovae are the explosions of heavily stripped massive stars which lost their envelopes via binary interactions with a compact companion star. They eject only ∼ 0.1 M ⊙ and may be the main way to form double neutronstar systems which eventually merge emitting strong gravitational waves. We follow the evolution of an ultra-stripped supernova progenitor until iron core collapse and perform explosive nucleosynthesis calculations. We then synthesize light curves and spectra of ultra-stripped supernovae using the nucleosynthesis results and present their expected properties. Ultra-stripped supernovae synthesize ∼ 0.01 M ⊙ of radioactive 56 Ni, and their typical peak luminosity is around 10 42 erg s −1 or −16 mag. Their typical rise time is 5 − 10 days. Comparing synthesized and observed spectra, we find that SN 2005ek, some of the so-called calcium-rich gap transients, and SN 2010X may be related to ultra-stripped supernovae. If these supernovae are actually ultra-stripped supernovae, their event rate is expected to be about 1 per cent of core-collapse supernovae. Comparing the double neutron-star merger rate obtained by future gravitational-wave observations and the ultra-stripped supernova rate obtained by optical transient surveys identified with our synthesized light-curve and spectral models, we will be able to judge whether ultra-stripped supernovae are actually a major contributor to the binary neutron star population and provide constraints on binary stellar evolution.

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Evolution of Progenitors for Electron Capture Supernovae

Cited by 90 publications

References 45 publications

Ultra-stripped supernovae: progenitors and fate

Ultra-stripped supernovae: progenitors and fate

Neutrino-driven explosions of ultra-stripped Type Ic supernovae generating binary neutron stars

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

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