Type Ia supernovae with and without blueshifted narrow Na i D lines – how different is their structure?

Hachinger, Stephan; Röpke, F. K.; Mazzali, P. A.; Gal‐Yam, A.; Maguire, K.; Sullivan, M.; Taubenberger, S.; Ashall, C.; Campbell, H.; Elias‐Rosa, N.; Feindt, U.; Greggio, L.; Inserra, C.; Miluzio, M.; Smartt, S. J.; Young, D. R.

doi:10.1093/mnras/stx1578

Cited by 4 publications

(1 citation statement)

References 111 publications

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“…There are also some statistical studies showing blueshifted narrow absorption features of Na I D in the high-resolution spectra of some SNe Ia (Sternberg et al 2011;Maguire et al 2013;Sternberg et al 2014), which are associated with the subclass characterized by higher photospheric velocities (Wang et al 2009b(Wang et al , 2013. Both results indicate that some SNe Ia are surrounded by CSM, favoring their SD progenitor system origin (Foley et al 2012;Hachinger et al 2017).…”

Section: Introductionmentioning

confidence: 92%

Observations of Type Ia Supernova 2014J for Nearly 900 Days and Constraints on Its Progenitor System

Li¹,

Yang

et al. 2019

ApJ

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We present extensive ground-based and Hubble Space T elescope (HST ) photometry of the highly reddened, very nearby type Ia supernova (SN Ia) 2014J in M82, covering the phases from 9 days before to about 900 days after the B-band maximum. SN 2014J is similar to other normal SNe Ia near the maximum light, but it shows flux excess in the B band in the early nebular phase. This excess flux emission can be due to light scattering by some structures of circumstellar materials located at a few 10 17 cm, consistent with a single degenerate progenitor system or a double degenerate progenitor system with mass outflows in the final evolution or magnetically driven winds around the binary system. At t∼+300 to ∼+500 days past the B-band maximum, the light 2 Li et al.curve of SN 2014J shows a faster decline relative to the 56 Ni decay. Such a feature can be attributed to the significant weakening of the emission features around [Fe III] λ4700 and [Fe II] λ5200 rather than the positron escape as previously suggested. Analysis of the HST images taken at t>600 days confirms that the luminosity of SN 2014J maintains a flat evolution at the very late phase. Fitting the late-time pseudo-bolometric light curve with radioactive decay of 56 Ni, 57 Ni and 55 Fe isotopes, we obtain the mass ratio 57 Ni/ 56 Ni as 0.035 ± 0.011, which is consistent with the corresponding value predicted from the 2D and 3D delayed-detonation models. Combined with early-time analysis, we propose that delayed-detonation through single degenerate scenario is most likely favored for SN 2014J.

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Section: Introductionmentioning

confidence: 92%

Observations of Type Ia Supernova 2014J for Nearly 900 Days and Constraints on Its Progenitor System

Li¹,

Yang

et al. 2019

ApJ

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Type Ia Supernova Explosions in Binary Systems: A Review

Liu

Roepke

Han

2023

Res. Astron. Astrophys.

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Type Ia supernovae (SNe Ia) play a key role in the fields of astrophysics and cosmology. It is widely accepted that SNe Ia arise from thermonuclear explosions of white dwarfs (WDs) in binary systems. However, there is no consensus on the fundamental aspects of the nature of SN Ia progenitors and their actual explosion mechanism. This fundamentally flaws our understanding of these important astrophysical objects. In this review, we outline the diversity of SNe Ia and the proposed progenitor models and explosion mechanisms. We discuss the recent theoretical and observational progress in addressing the SN Ia progenitor and explosion mechanism in terms of the observables at various stages of the explosion, including rates and delay times, pre-explosion companion stars, ejecta-companion interaction, early excess emission, early radio/X-ray emission from circumstellar material (CSM) interaction, surviving companion stars, late-time spectra and photometry, polarization signals, and supernova remnant properties, etc. Despite the efforts from both the theoretical and observational side, the questions of how the WDs reach an explosive state and what progenitor systems are more likely to produce SNe Ia remain open. No single published model is able to consistently explain all observational features and the full diversity of SNe Ia. This may indicate that either a new progenitor paradigm or the improvement of current models is needed if all SNe Ia arise from the same origin. An alternative scenario is that different progenitor channels and explosion mechanisms contribute to SNe Ia. In the next decade, the ongoing campaigns with the James Webb Space Telescope (JWST), Gaia and the Zwicky Transient Facility (ZTF), and upcoming extensive projects with the Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST) and the Square Kilometre Array (SKA) will allow us to conduct not only studies of individual SNe Ia in unprecedented detail but also systematic investigations for different subclasses of SNe Ia. This will advance theory and observations of SNe Ia sufficiently far to gain a deeper understanding of their origin and explosion mechanism.

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Dalek: A Deep Learning Emulator for TARDIS

Kerzendorf

Vogl

Buchner

et al. 2021

ApJL

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Supernova spectral time series contain a wealth of information about the progenitor and explosion process of these energetic events. The modeling of these data requires the exploration of very high dimensional posterior probabilities with expensive radiative transfer codes. Even modest parameterizations of supernovae contain more than 10 parameters and a detailed exploration demands at least several million function evaluations. Physically realistic models require at least tens of CPU minutes per evaluation putting a detailed reconstruction of the explosion out of reach of traditional methodology. The advent of widely available libraries for the training of neural networks combined with their ability to approximate almost arbitrary functions with high precision allows for a new approach to this problem. Instead of evaluating the radiative transfer model itself, one can build a neural network proxy trained on the simulations but evaluating orders of magnitude faster. Such a framework is called an emulator or surrogate model. In this work, we present an emulator for the tardis supernova radiative transfer code applied to Type Ia supernova spectra. We show that we can train an emulator for this problem given a modest training set of 100,000 spectra (easily calculable on modern supercomputers). The results show an accuracy on the percent level (that are dominated by the Monte Carlo nature of tardis and not the emulator) with a speedup of several orders of magnitude. This method has a much broader set of applications and is not limited to the presented problem.

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Type Ia supernovae with and without blueshifted narrow Na i D lines – how different is their structure?

Cited by 4 publications

References 111 publications

Observations of Type Ia Supernova 2014J for Nearly 900 Days and Constraints on Its Progenitor System

Observations of Type Ia Supernova 2014J for Nearly 900 Days and Constraints on Its Progenitor System

Type Ia Supernova Explosions in Binary Systems: A Review

Dalek: A Deep Learning Emulator for TARDIS

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