How much H and He is ‘hidden’ in SNe Ib/c? – I. Low-mass objects

By Stephan Hachinger, P. Mazzali, Stefan Taubenberger, W. Hillebrandt, K. Nomoto, Daniel Sauer. 2012

144 citations recorded by the source corpus.

H and He features in photospheric spectra have seldom been used to infer quantitatively the properties of Type IIb, Ib and Ic supernovae (SNe IIb, Ib and Ic) and their progenitor stars. Most radiative transfermodels ignored non-local thermodynamic equilibrium (NLTE) effects, which are extremely strong especially in the He-dominated zones. In this paper, a comprehensive set of model atmospheres for low-mass SNe IIb/Ib/Ic is presented. Long-standing questions, such as how much He can be contained in SNe Ic, where He lines are not seen, can thus be addressed. The state of H and He is computed in full NLTE, including the effect of heating by fast electrons. The models are constructed to represent iso-energetic explosions of the same stellar core with differently massive H/He envelopes on top. The synthetic spectra suggest that 0.06-0.14 M-circle dot of He and even smaller amounts of H suffice for optical lines to be present, unless ejecta asymmetries play a major role. This strongly supports the conjecture that low-mass SNe Ic originate from binaries where progenitor mass loss can be extremely efficient.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/c1de95b5c5f7e4fb16ce4f0e6cc38cef48f6ac8b

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In Astronomy and Astrophysics

1. S. Smartt
2. N. Smith
3. A. Filippenko
4. Stan Woosley
5. Ryan Chornock
6. E. Berger
7. R. Kirshner
8. S. Jha

In Instrumentation

1. N. Smith
2. A. Filippenko
3. S. Smartt
4. J. Silverman
5. N. Langer
6. A. Chieffi
7. M. Limongi
8. Ryan Chornock

In Statistical and Nonlinear Physics

1. A. Chieffi
2. M. Limongi
3. N. Smith
4. A. Gal-yam
5. Jay Anderson
6. Richard S. Ellis
7. N. Langer
8. J. Silverman

Citations in the corpus

• DISCOVERY, PROGENITOR AND EARLY EVOLUTION OF A STRIPPED ENVELOPE SUPERNOVA iPTF13bvn (2013, background): “Helium lines are not expected to be prominent in early spectra of Type Ib supernovae (Hachinger et al. 2012).”
• Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, background): “…457, 328–350 (2016) D ow nloaded from https://academ ic.oup.com /m nras/article/457/1/328/989045 by guest on 14 January 2021 has been widely debated (e.g. Branch et al. 2002; Folatelli et al. 2006; Parrent et al. 2007; Tanaka et al. 2009; Hachinger et al. 2012; Parrent et al. 2015).”
• A new method for estimating the bolometric properties of Ibc supernovae (2013, background): “However, Hachinger et al. (2012) have shown that only 0.06− 0.14 M of helium is required in the ejecta to be present in the observed spectra of Ib SNe, which accounts to only a small percentage of the total ejecta masses in Ibc SNe (which are of order several solar masses) and therefore may not…”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, background): “The collective conclusion of these observational investigations states that the lack of helium features in SNe Ic spectra cannot be attributed to poor mixing but rather the absence of this element in the ejecta, which agrees with the conclusion of [268] that no more than 0.”
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “However, Smith et al. (2011b) pointed out that the relevant ratio really is (IIb + Ibc)/(II-P + II-L + IIn), since SNe IIb are almost identical to SNe Ib but for <0.01 M⊙ of H in their outermost layer (Dessart et al. 2011, Hachinger et al. 2012).”
• Hubble Space Telescope spectra of the type Ia supernova SN 2011fe: a tail of low-density, high-velocity material with Z < Z⊙ (2013, background): “The line velocities reflect the time evolution of the density profile, and thus in particular the assumed tr (Hachinger et al. 2012).”
• PTF12os and iPTF13bvn. Two stripped-envelope supernovae from low-mass progenitors in NGC 5806 (2016, background): “In the modeling effort by Hachinger et al. (2012), it was found that as little as 0.024 M of hydrogen in the envelope is enough for Hβ (and a strong signal from Hα) to show up in the spectra of a SN IIb/Ib; thus, a hydrogen envelope mass upper limit of .0.02 M is a reasonable estimate for PTF12os…”
• Ultra-stripped supernovae: progenitors and fate (2015, methodology): “The modelling of synthetic SN spectra by Hachinger et al. (2012) suggests that more than0.”
• OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, background): “…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 spectroscopic (e.g., Howell et al. 2005; Blondin &…”
• Presupernova Evolution and Explosive Nucleosynthesis of Rotating Massive Stars in the Metallicity Range −3 ≤ [Fe/H] ≤ 0 (2018, methodology): “5 (column 6); the angular momenta contained within the iron core (column 7), the CO core (column 8), the He core (column 9), the inner 1.5Me (column 10), and the inner 2.0Me (column 11); and the expected SN type, according to the classification suggested by Hachinger 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).”
• PRE-SUPERNOVA EVOLUTION OF ROTATING SOLAR METALLICITY STARS IN THE MASS RANGE 13–120 M☉ AND THEIR EXPLOSIVE YIELDS (2012, methodology): “Note that, in order to classify the various core collapse supernovae we adopted the following H and He limiting masses (see also Hachinger et al. 2012): (1) M(H)min,SNIIP ≃ 0.3 M⊙ (the minimum H mass for a Type IIP SN); (2) M(H)min,SNIIb ≃ 0.1 M⊙ (the minimum H mass for a Type IIb SN); (3)…”
• RADIATIVE TRANSFER SIMULATIONS OF NEUTRON STAR MERGER EJECTA (2013, background): “In fact, non-thermal effects are known to be important for the excitation of He lines in Type Ib SNe (Lucy 1991; Dessart et al. 2011; Hachinger et al. 2012).”
• TYPE Iax SUPERNOVAE: A NEW CLASS OF STELLAR EXPLOSION (2012, background): “For instance, an outstanding question is how much helium exists in the ejecta of SNe Ic (e.g., Hachinger et al. 2012).”