TYPE Ib/c SUPERNOVAE IN BINARY SYSTEMS. I. EVOLUTION AND PROPERTIES OF THE PROGENITOR STARS

By Sung-Chul Yoon, Stan Woosley, N. Langer. 2010

253 citations recorded by the source corpus.

We investigate the evolution of Type Ib/c supernova (SN Ib/c) progenitors in close binary systems, using new evolutionary models that include the effects of rotation, with initial masses of 12–25 M☉ for the primary components, and of single helium stars with initial masses of 2.8–20 M☉. We find that, despite the impact of tidal interaction on the rotation of primary stars, the amount of angular momentum retained in the core at the presupernova stage in different binary model sequences converges to a value similar to those found in previous single star models. This amount is large enough to produce millisecond pulsars, but too small to produce magnetars or long gamma-ray bursts. We employ the most up-to-date estimate for the Wolf-Rayet mass-loss rate, and its implications for SN Ib/c progenitors are discussed in detail. In terms of stellar structure, SN Ib/c progenitors in binary systems at solar metallicity are predicted to have a wide range of final masses up to about 7 M☉, with helium envelopes of MHe ≃ 0.16–1.5 M☉. Our results indicate that, if the lack of helium lines in the spectra of SNe Ic were due to small amounts of helium (e.g., MHe ≲ 0.5), the distribution of both initial and final masses of SN Ic progenitors should be bimodal. Furthermore, we find that a thin hydrogen layer (0.001 M☉ ≲ MH ≲ 0.01 M☉) is expected to be present in many SN Ib progenitors at the presupernova stage. We show that the presence of hydrogen, together with a rather thick helium envelope, can lead to a significant expansion of some SN Ib/c progenitors by the time of supernova explosion. This may have important consequences for the shock break-out and supernova light curve. We also argue that some SN progenitors with thin hydrogen layers produced via Case AB/B transfer might be related to Type IIb supernova progenitors with relatively small radii of about 10 R☉.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/48039776bf2e29d1f76119fd465f65c92f5aab3f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

How much H and He is ‘hidden’ in SNe Ib/c? – I. Low-mass objects (2012, background): “2007) and the progenitor stars (Georgy et al. 2009; Smartt 2009; Yoon et al. 2010) are progressively being resolved.”
Grids of stellar models with rotation - II. WR populations and supernovae/GRB progenitors at Z = 0.014 (2012, background): “Close-binary scenarios of Yoon et al. (2010) actually predict a bimodal distribution for the progenitors of type Ic: the high-mass progenitors (initial masses greater than 35 – 45M⊙) and the low-mass progenitors (between 12.5 – 13.5 M⊙).”
The spin of the second-born black hole in coalescing binary black holes (2018, methodology): “Black dotted line corresponds to the formula from Yoon et al. (2010); red dashed line refers to the free fitting; green solid line refers to the fitting data with the fixed exponent of Rconv/R = 8.0, cyan dotted line refers to the fitting data with all three different metallicities.”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): PLANETS, OSCILLATIONS, ROTATION, AND MASSIVE STARS (2013, background): “Following Yoon et al. (2010) we limit the mass loss timescale to the thermal timescale of the star τKH Ṁ = min [ Ṁ(Ω) , f M τKH ] (27) where f is an efficiency factor of order unity (default value is f = 0.3).”
The death of massive stars – I. Observational constraints on the progenitors of Type II-P supernovae (2008, background): “The strongest case for binary stars contributing to the Type Ib/c SN progenitor populations can be made by the fact we can reproduce the observed relative rate of different SN types (Podsiadlowski et al. 1992; De Donder & Vanbeveren 1998; Yoon et al. 2010).”
On the nature of supernovae Ib and Ic (2012, methodology): “Inefficient non-thermal excitation of He I may result from (1) helium deficiency or underabundance (Yoon et al. 2010 argues for the possibility of even lower mass helium-deficient progenitors than those presented here); (2) a higher mass helium core with a sizeable oxygen-rich mass buffer, which…”
The Carnegie Supernova Project I: analysis of stripped-envelope supernova light curves (2017, background): “For relatively low initial-mass stars, to strip the outer hydrogen layers, and in the case of SNe Ic, also the helium envelopes, mass transfer to a companion star is required (see e.g., Yoon et al. 2010).”
Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey (2014, result): “…are in agreement with the values expected for hot and massive (MZAMS > 25 M ) Wolf-Rayet stars, which are stripped of their hydrogen-rich envelopes by strong line-driven winds, but also with the radii of stars which were initially less massive and were stripped by a companion (Yoon et al. 2010).”
Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars (2016, background): “…companions can evolve to produce X-ray binaries (Verbunt 1993), millisecond pulsars (Lorimer 2008), Type Ia (Wang & Han 2012) and possibly Type Ib/c (Yoon et al. 2010) supernovae, Algols (van Rensbergen et al. 2011), short (Nakar 2007) and perhaps long (Izzard et al. 2004) gamma ray bursts,…”
Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, methodology): “Another commonly used binary star code is based on the original Kippenhahn code, exemplified by the Bonn Evolu- tionary Code (BEC, Heger, Langer, & Woosley 2000; Yoon et al. 2010).”
Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction (2017, methodology): “Pioneers in modeling the effects on (samples of) ccSNe include Podsiadlowski et al. (1992), De Donder & Vanbeveren (2003b), Yoon et al. (2010), Eldridge et al. (2008, 2013).”
A new method for estimating the bolometric properties of Ibc supernovae (2013, background): “…arise from in the in-spiral of a compact object into the core of a massive companion star cannot be ruled out, though it should be considered that Yoon et al. (2010) have shown that the angular momentum retained by the exploding star in the binary system is not enough to produce a magnetar nor a…”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, methodology): “The interior evolution and the final mass transfer were calculated using the binary evolution code BEC (Wellstein et al. 2001; Yoon et al. 2010) until after the detachment of the binary.”
Progenitors of gravitational wave mergers: binary evolution with the stellar grid-based code ComBinE (2018, methodology): “The underlying stellar models are calculated with the stellar evolution code BEC (e.g. Yoon et al. 2010, and references therein).”
OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, background): “…(see our companion paper, M. Modjaz et al., in preparation), as well as for comparisons to theoretical models and radiative transfer codes (e.g., Yoon et al. 2010; Dessart et al. 2011; Hachinger et al. 2012; Dessart et al. 2012) and for inclusions in SN identification schemes, both…”