On the brightness distribution of Type Ia supernovae from violent white dwarf mergers

Ruiter, Ashley J.; Sim, Stuart; Pakmor, Rüdiger; Kromer, M.; Seitenzahl, Ivo R.; Belczyński, K.; Fink, Michael; Herzog, Matthias; Hillebrandt, W.; Röpke, F. K.; Taubenberger, S.

doi:10.1093/mnras/sts423

Cited by 120 publications

(184 citation statements)

References 68 publications

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“…see Woosley & Weaver 1994). This scenario is attractive since it can account for the progenitor statistics from population synthesis (see Livio 2000;Ruiter et al 2013). Moreover, studies like Stritzinger et al (2006a) and Scalzo et al (2014) find a significant fraction of SNe Ia to have M ej < 1.4 M , providing observational evidence for the sub-M Ch progenitor scenario.…”

Section: M56 Nimentioning

confidence: 98%

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A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

Dhawan

Leibundgut

Spyromilio

et al. 2016

A&A

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The increase in the number of Type Ia supernovae (SNe Ia) has demonstrated that the population shows greater diversity than has been assumed in the past. The reasons (e.g. parent population, explosion mechanism) for this diversity remain largely unknown. We investigated a sample of SNe Ia near-infrared light curves and correlated the phase of the second maximum with the bolometric peak luminosity. The peak bolometric luminosity is related to the time of the second maximum (relative to the B light curve maximum) as follows: L max (10 43 erg s −1 ) = (0.039 ± 0.004) × t 2 (J)(days) + (0.013 ± 0.106). 56 Ni masses can be derived from the peak luminosity based on Arnett's rule, which states that the luminosity at maximum is equal to the instantaneous energy generated by the nickel decay. We checked this assumption against recent radiative-transfer calculations of Chandrasekhar-mass delayed detonation models and find this assumption is valid to within 10% in recent radiative-transfer calculations of Chandrasekhar-mass delayed detonation models. The L max vs. t 2 relation is applied to a sample of 40 additional SNe Ia with significant reddening (E(B − V) > 0.1 mag), and a reddening-free bolometric luminosity function of SNe Ia is established. The method is tested with the 56 Ni mass measurement from the direct observation of γ-rays in the heavily absorbed SN 2014J and found to be fully consistent. Super-Chandrasekhar-mass explosions, in particular SN 2007if, do not follow the relations between peak luminosity and second IR maximum. This may point to an additional energy source contributing at maximum light. The luminosity function of SNe Ia is constructed and is shown to be asymmetric with a tail of low-luminosity objects and a rather sharp high-luminosity cutoff, although it might be influenced by selection effects.

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Section: M56 Nimentioning

confidence: 98%

“…We compare the luminosity function in Fig. 3 to the one obtained by Ruiter et al (2013), using their violent merger models. They present a relation between primary white dwarf mass (M WD ) and peak brightness for a grid of sub-M Ch models.…”

Section: M56 Nimentioning

confidence: 99%

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

Dhawan

Leibundgut

Spyromilio

et al. 2016

A&A

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“…The SN Ia peak brightness in their simulations is directly related to the WD explosion mass. We apply the M WD − M bol relationship found by Ruiter et al (2013) to derive the SN Ia peak brightness.…”

Section: Luminosity Distributionmentioning

confidence: 99%

Producing Type Iax supernovae from a specific class of helium-ignited WD explosions

Wang

Justham

Han

2013

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Context. It has recently been proposed that one subclass of Type Ia supernovae (SNe Ia) is sufficiently distinct and sufficiently common to be classified separately from the bulk of SNe Ia; the suggested class name is Type Iax supernovae (SNe Iax), after SN 2002cx. However, their progenitors are still uncertain. Aims. We study whether the population properties of this class might be understood if the events originate from a subset of subChandrasekhar mass explosions. In this potential progenitor population, a carbon-oxygen white dwarf (CO WD) accumulates a helium layer from a non-degenerate helium star; ignition of that helium layer then leads to ignition of the CO WD. Methods. We incorporated detailed binary evolution calculations for the progenitor systems into a binary population synthesis model to obtain rates and delay times for these events. Results. The predicted Galactic event rate of these explosions is ∼1.5 × 10 −3 yr −1 according to our standard model, in good agreement with the measured rates of SNe Iax. In addition, predicted delay times are ∼70 Myr−800 Myr, consistent with the fact that most of SNe Iax have been discovered in late-type galaxies. If the explosions are assumed to be double detonations -following current model expectations -then, based on the CO WD masses at explosion, we also estimate the distribution of resulting SN brightness (−13 > ∼ M bol > ∼ −19 mag), which can reproduce the empirical diversity of SNe Iax. Conclusions. We speculate on why binaries with non-degenerate donor stars might lead to SNe Iax if similar systems with degenerate donors do not. We suggest that the high mass of the helium layer necessary for ignition at the lower accretion rates typically delivered from non-degenerate donors might be necessary to produce SN 2002cx-like characteristics, perhaps even by changing the nature of the CO ignition.

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“…The manner in which the exploding, probably carbonoxygen (CO), white dwarf (WD) accretes matter in the first place and the nature of the companion have been topics of debate for decades (Whelan & Iben 1973;Nomoto 1982;Iben & Tutukov 1984;Webbink 1984;Yungelson et al 1995;Tutukov & Yungelson 1996;Yungelson & Livio 2000;Han & Podsiadlowski 2004;Ruiter et al 2009Ruiter et al , 2013Mennekens et al 2010;Toonen et al 2012;Hillebrandt et al 2013).…”

Section: Introductionmentioning

confidence: 99%

“…Furthermore, the fact that only a few per cent of SNe Ia are classified as 1991T-like (Li et al 2011;Silverman et al 2012;Blondin et al 2012) would be naturally explained by the relative scarcity of the single-degenerate scenario compared to the violent-merger or double-detonation scenarios (e.g. Ruiter et al 2009Ruiter et al , 2011Ruiter et al , 2013Fisher & Jumper 2015). The identification of GCD explosions with SNe 91T is challenged from observations of the supernova remnant SNR 0509-67.5 in the LMC.…”

Section: Introductionmentioning

confidence: 99%

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

Seitenzahl

Kromer

Ohlmann

et al. 2016

A&A

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The gravitationally confined detonation (GCD) model has been proposed as a possible explosion mechanism for Type Ia supernovae in the single-degenerate evolution channel. It starts with ignition of a deflagration in a single off-centre bubble in a near-Chandrasekharmass white dwarf. Driven by buoyancy, the deflagration flame rises in a narrow cone towards the surface. For the most part, the main component of the flow of the expanding ashes remains radial, but upon reaching the outer, low-pressure layers of the white dwarf, an additional lateral component develops. This causes the deflagration ashes to converge again at the opposite side, where the compression heats fuel and a detonation may be launched. We first performed five three-dimensional hydrodynamic simulations of the deflagration phase in 1.4 M carbon/oxygen white dwarfs at intermediate-resolution (256 3 computational zones). We confirm that the closer the initial deflagration is ignited to the centre, the slower the buoyant rise and the longer the deflagration ashes takes to break out and close in on the opposite pole to collide. To test the GCD explosion model, we then performed a high-resolution (512 3 computational zones) simulation for a model with an ignition spot offset near the upper limit of what is still justifiable, 200 km. This high-resolution simulation met our deliberately optimistic detonation criteria, and we initiated a detonation. The detonation burned through the white dwarf and led to its complete disruption. For this model, we determined detailed nucleosynthetic yields by post-processing 10 6 tracer particles with a 384 nuclide reaction network, and we present multi-band light curves and time-dependent optical spectra. We find that our synthetic observables show a prominent viewing-angle sensitivity in ultraviolet and blue wavelength bands, which contradicts observed SNe Ia. The strong dependence on the viewing angle is caused by the asymmetric distribution of the deflagration ashes in the outer ejecta layers. Finally, we compared our model to SN 1991T. The overall flux level of the model is slightly too low, and the model predicts pre-maximum light spectral features due to Ca, S, and Si that are too strong. Furthermore, the model chemical abundance stratification qualitatively disagrees with recent abundance tomography results in two key areas: our model lacks low-velocity stable Fe and instead has copious amounts of high-velocity 56 Ni and stable Fe. We therefore do not find good agreement of the model with SN 1991T.

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On the brightness distribution of Type Ia supernovae from violent white dwarf mergers

Cited by 120 publications

References 68 publications

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

Producing Type Iax supernovae from a specific class of helium-ignited WD explosions

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

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On the brightness distribution of Type Ia supernovae from violent white dwarf mergers

Cited by 120 publications

References 68 publications

A reddening-free method to estimate the56Ni mass of Type Ia supernovae

A reddening-free method to estimate the56Ni mass of Type Ia supernovae

Producing Type Iax supernovae from a specific class of helium-ignited WD explosions

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

Contact Info

Product

Resources

About

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae

A reddening-free method to estimate the⁵⁶Ni mass of Type Ia supernovae