3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae★

Kromer, M.; Fink, Michael; Stanishev, V.; Taubenberger, S.; Ciaraldi-Schoolmann, Franco; Pakmor, Rüdiger; Röpke, F. K.; Ruiter, Ashley J.; Seitenzahl, Ivo R.; Sim, Stuart; Blanc, G.; Elias‐Rosa, N.; Hillebrandt, W.

doi:10.1093/mnras/sts498

Cited by 211 publications

(352 citation statements)

References 75 publications

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“…To corroborate this result and to place further constraints on the relative fractions of near-M Ch and sub-M Ch WD primaries, we consider five pend on progenitor metallicity (using models N100_Z0.01, N100_Z0.1, and N100 from Seitenzahl et al 2013). -case sub-M Ch +2002cx: 20% of SNe Ia explode as pure deflagrations leaving remnants (model N5def from Kromer et al 2013), and the remaining 80% explode as in case sub-M Ch . In Fig.…”

Section: Resultsmentioning

confidence: 99%

Solar abundance of manganese: a case for near Chandrasekhar-mass Type Ia supernova progenitors

Seitenzahl

Cescutti

Röpke

et al. 2013

A&A

162

194

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Context. Manganese is predominantly synthesised in Type Ia supernova (SN Ia) explosions. Owing to the entropy dependence of the Mn yield in explosive thermonuclear burning, SNe Ia involving near Chandrasekhar-mass (M Ch ) white dwarfs (WDs) are predicted to produce Mn-to-Fe ratios that significantly exceed those of SN Ia explosions involving sub-Chandrasekhar mass primary WDs. Of all current supernova explosion models, only SN Ia models involving near-M Ch WDs produce [Mn/Fe] 0.0. Aims. Using the specific yields for competing SN Ia scenarios, we aim to constrain the relative fractions of exploding near-M Ch to sub-M Ch primary WDs in the Galaxy. Methods. We extract the Mn yields from three-dimensional thermonuclear supernova simulations that refer to different initial setups and progenitor channels. We then compute the chemical evolution of Mn in the solar neighborhood, assuming SNe Ia are made up of different relative fractions of the considered explosion models. Results. We find that due to the entropy dependence of freeze-out yields from nuclear statistical equilibrium, [Mn/Fe]

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Section: Resultsmentioning

confidence: 99%

Solar abundance of manganese: a case for near Chandrasekhar-mass Type Ia supernova progenitors

Seitenzahl

Cescutti

Röpke

et al. 2013

A&A

162

194

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“…This means that GCD explosions are automatically linked to the brighter end of the SN Ia distribution. If the WD were ignited closer to the centre, we would obtain a stronger deflagration, resulting in stronger expansion, no detonation, and a sub-luminous SN 2002cx-like event (Jordan et al 2012b;Kromer et al 2013).…”

Section: Discussionmentioning

confidence: 99%

“…The network employs the reaction rates from the JINA database (Cyburt et al 2010) as of January 27, 2014. As outlined in Kromer et al (2013), we implemented the effects of solar metallicity of the progenitor by initializing the tracer particle composition to 50% 16 O, 48.29% 12 C, and the remaining 1.71% of the mass to the solar composition from Asplund et al (2009) for elements heavier than He, with the exception of solar C, N, O, which we converted into 22 Ne to account for the effects of core He-burning.…”

Section: Nucleosynthesismentioning

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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“…Indeed NIR spectra of the spectroscopic defined SNe Iax class are nearly nonexistent, with the only published observations being those consisting of a sequence of five epochs taken of the bright SN 2005hk (peak M V ∼ −18 mag; Phillips et al 2007), which were recently presented by Kromer et al (2013). Making use of a subset of that unique data set, plotted in the right panel of Fig.…”

Section: Spectral Comparison Of Sn 2010ae To Relevant Sne Iaxmentioning

confidence: 99%

Optical and near-IR observations of the faint and fast 2008ha-like supernova 2010ae

Stritzinger

Hsiao

Valenti

et al. 2014

A&A

171

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A comprehensive set of optical and near-infrared (NIR) photometry and spectroscopy is presented for the faint and fast 2008ha-like supernova (SN) 2010ae. Contingent on the adopted value of host extinction, SN 2010ae reached a peak brightness of −13.8 > M V > −15.3 mag, while modeling of the UVOIR light curve suggests it produced 0.003-0.007 M of 56 Ni, ejected 0.30−0.60 M of material, and had an explosion energy of 0.04-0.30 × 10 51 erg. The values of these explosion parameters are similar to the peculiar SN 2008ha -for which we also present previously unpublished early phase optical and NIR light curves -and places these two transients at the faint end of the 2002cx-like SN population. Detailed inspection of the post-maximum NIR spectroscopic sequence indicates the presence of a multitude of spectral features, which are identified through SYNAPPS modeling to be mainly attributed to Co ii. Comparison with a collection of published and unpublished NIR spectra of other 2002cx-like SNe, reveals that a Co ii footprint is ubiquitous to this subclass of transients, providing a link to Type Ia SNe. A visual-wavelength spectrum of SN 2010ae obtained at +252 days past maximum shows a striking resemblance to a similar epoch spectrum of SN 2002cx. However, subtle differences in the strength and ratio of calcium emission features, as well as diversity among similar epoch spectra of other 2002cx-like SNe indicates a range of physical conditions of the ejecta, highlighting the heterogeneous nature of this peculiar class of transients.

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3D deflagration simulations leaving bound remnants: a model for 2002cx-like Type Ia supernovae★

Cited by 211 publications

References 75 publications

Solar abundance of manganese: a case for near Chandrasekhar-mass Type Ia supernova progenitors

Solar abundance of manganese: a case for near Chandrasekhar-mass Type Ia supernova progenitors

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

Optical and near-IR observations of the faint and fast 2008ha-like supernova 2010ae

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