On the nature of supernovae Ib and Ic

By L. Dessart, D. John Hillier, Chengdong Li, Stan Woosley. 2012

169 citations recorded by the source corpus.

Utilizing non-local thermodynamic equilibrium time-dependent radiative-transfer calculations, we investigate the impact of mixing and non-thermal processes associated with radioactive decay on Type IIb/Ib/Ic supernova (SN IIb/Ib/Ic) light curves and spectra. Starting with short-period binary models of ≾5M_⊙ helium-rich stars, originally 18 and 25M_⊙ on the main sequence, we produce 1.2B ejecta which we artificially mix to alter the chemical stratification. While the total ^(56)Ni mass influences the light-curve peak, the spatial distribution of ^(56)Ni, controlled by mixing processes, impacts both the multiband light curves and spectra. With enhanced γ-ray escape. Non-thermal electrons, crucial for the production of He_I lines, deposit a large fraction of their energy as heat, and this fraction approaches 100 per cent under fully ionized conditions. Because energy deposition is generally local well after the light-curve peak, the broad He_I line characteristics of maximum-light SN IIb/Ib spectra require mixing that places ^(56)Ni and helium nuclei to within a γ-ray mean free path. This requirement indicates that SNe IIb and Ib most likely arise from the explosions of stripped-envelope massive stars (main-sequence masses ≾25M_⊙) that have evolved through mass transfer in a binary system, rather than from more massive single Wolf-Rayet stars. In contrast, the lack of He_I lines in SNe Ic may result from a variety of causes: a genuine helium deficiency; strongly asymmetric mixing; weak mixing; or a more massive, perhaps single, progenitor characterized by a larger oxygen-rich core. Helium deficiency is not a prerequisite for SNe Ic. Our models, subject to different mixing magnitudes, can produce a variety of SN types, including IIb, IIc, Ib and Ic. As it is poorly constrained by explosion models, mixing challenges our ability to infer the progenitor and explosion properties of SNe IIb/Ib/Ic.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/930df94a3061daa6dc36a6f2b94b755e259d54f3

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In Astronomy and Astrophysics

1. S. Smartt
2. N. Smith
3. Stan Woosley
4. A. Filippenko
5. B. Metzger
6. S. Valenti
7. N. Langer
8. Hans-Thomas Janka

Citations in the corpus

• CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, background): “For example, it seems most likely that common SNe Ib and Icresult from binary systems containing stars whose pre-SN mass is only 3 or 4 M (Ensman & Woosley 1988; Dessart et al. 2012).”
• The Evolution of Massive Helium Stars, Including Mass Loss (2019, result): “Previous studies of models in this mass range have shown good agreement with observations (Dessart et al. 2012, 2016).”
• OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, methodology): “…1994; Clocchiatti et al. 1996; Matheson et al. 2001, and more recently, e.g., Modjaz et al. 2009; Leloudas et al. 2011; Dessart et al. 2011; Hachinger et al. 2012; Dessart et al. 2012, and for SNe IIb, see Pastorello et al. 2008; Chornock et al. 2011; Arcavi et al. 2011; Milisavljevic et al. 2013).”
• Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, background): “The amount of mixing will affect the rise time of the SNe since radiation from high-velocity (i.e. further out in radius, given homologous expansion) 56Ni will have a shorter diffusion time (Maeda et al. 2003; Dessart et al. 2012).”
• Evolution and fate of very massive stars (2013, background): “We can now see how our models compare with observed superluminous SNe (SLSNe).”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, background): “A prediction of RTmodels [270] is if the lack of mixing is the only discriminant between SNe Ib and Ic, then well-mixed SNe Ib should have higher ejecta velocities than the less well-mixed SNe Ic.”
• Observational and Physical Classification of Supernovae (2016, unknown): “…idea would be that SNe Ib and SNe Ic actually arise from physically similar progenitors, and differ only in the post-supernova photospheric conditions, that are conductive to the formation of He lines in SNe Ib, but not in SNe Ic (e.g., due to weaker radioactive 56Ni mixing; Dessart et al. 2012).”
• Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey (2014, background): “Moreover, a strongly mixed SN has a shorter light curve rise time 20 than a poorly mixed one, as reported by Dessart et al. (2012).”
• Luminous blue variables are antisocial: their isolation implies that they are kicked mass gainers in binary evolution (2014, methodology): “Similar arguments in favor of binary progenitors have been made based on analyses of the mass and composition of the ejecta in stripped-envelope SNe (Dessart et al. 2012; Hachinger et al. 2012).”
• Type II-Plateau supernova radiation: dependences on progenitor and explosion properties (2013, methodology): “…Mg, Si, S, Ar, K, and Ca. (ii) Neglect of non-thermal processes: As demonstrated by Lucy (1991); Kozma & Fransson (1992, 1998a,b); Li et al. (2012); Dessart et al. (2012),γ-rays from radioactive decay give rise to high-energy electrons that can non-thermally excite and ioize the gas, exacerbating…”
• Superluminous supernovae: 56Ni power versus magnetar radiation (2012, methodology): “Spectroscopically, our PISN simulations reflect in many ways the properties of lower-mass lower-energy SNe II-P, II-pec, and Ib/c (Dessart et al. 2012).”
• PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 (2016, background): “Two main mechanisms have been suggested to produce SE SNe: either binary mass transfer (e.g., Iben & Tutukov 1985; Yoon et al. 2010; Claeys et al. 2011; Dessart et al. 2012; Yoon 2015) or strong line-driven winds from massive Wolf-Rayet (WR) stars (e.g., Conti 1976; Groh et al. 2013; Smith 2014).”
• A new method for estimating the bolometric properties of Ibc supernovae (2013, background): “It has been noted in the literature, including a recent paper by Dessart et al. (2012), that Ic-BL SNe, including GRB/XRF SNe, are associated with larger ejecta masses and kinetic energies than Ib and Ic SNe.”
• Delayed outflows from black hole accretion tori following neutron star binary coalescence (2013, methodology): “This is in analogy to the mechanism responsible for producing He lines in corecollapse SNe as the result of mixing radioactive 56Ni into the outer layers of the ejecta (e.g. Lucy 1991, Dessart et al. 2012).”
• DISCOVERY, PROGENITOR AND EARLY EVOLUTION OF A STRIPPED ENVELOPE SUPERNOVA iPTF13bvn (2013, background): “On theoretical grounds, the anticipated progenitors are Wolf Rayet (WR) stars or massive Helium stars (e.g., Dessart et al. 2012; Yoon et al. 2012).”