Intermediate luminosity type Iax supernova 2019muj with narrow absorption lines: Long-lasting radiation associated with a possible bound remnant predicted by the weak deflagration model

Kawabata, Miho; Maeda, Keiichi; Yamanaka, Masahito; Nakaoka, Tatsuya; Kawabata, Koji S.; Aoki, Kentaro; Anupama, G. C.; Burgaz, U.; Dutta, Anirban; Isogai, Keisuke; Kino, Motoki; Kojiguchi, Naoto; Iida, Katsuyoshi; Kumar, Brijesh; Kuroda, D.; Maehara, Hiroyuki; Matsubayashi, Kazuya; Morihana, K.; Murata, Katsuhiro L.; Ohshima, Tomohito; Otsuka, Masaaki; Sahu, D. K.; Singh, Avinash; Sugitani, Koji; Takahashi, Jun; Takagi, Kengo

doi:10.1093/pasj/psab075

Cited by 14 publications

(28 citation statements)

References 67 publications

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“…Unlike normal SNe Ia, they never enter into the pure nebular phase but keep showing the photospheric spectra dominated by allowed transitions (mainly Fe II) (Jha et al 2006;Sahu et al 2008;McCully et al 2014b;Foley et al 2016). This is qualitatively consistent with their light-curve properties, showing a slow evolution roughly following the 56 Co decay with little leakage of the decay γ-rays (or even slower) (Foley et al 2014;Kawabata et al 2018Kawabata et al , 2021McCully et al 2022). These latetime properties point to the existence of a high-density, innermost region.…”

Section: Introductionsupporting

confidence: 70%

“…These latetime properties point to the existence of a high-density, innermost region. It has been speculated that these properties may be associated with the putative WD remnant in the failed deflagration scenario (Foley et al 2016;Kawabata et al 2021), but the connection has not been established. Especially, the nature of the innermost region has not been clarified in a detailed and quantitative manner.…”

Section: Introductionmentioning

confidence: 99%

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Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core

Maeda

Kawabata

2022

ApJ

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Type Iax supernovae (SNe Iax) form a class of peculiar SNe Ia, whose early phase spectra share main spectral line identifications with canonical SNe Ia but with higher ionization and much lower line velocities. Their late-time behaviors deviate from usual SNe Ia in many respects; SNe Iax continue showing photospheric spectra over several 100 days and the luminosity decline is very slow. In this work, we study the late-time spectra of SN Iax 2019muj, including a newly presented spectrum at ∼500 days. The spectrum is still dominated by allowed transitions but with a lower ionization state, with possible detection of [O i]λλ6300, 6363. By comprehensively examining the spectral formation processes of allowed transitions (Fe ii, Fe i, and the Ca ii near-IR triplet) and forbidden transitions ([Ca ii]λλ7292, 7324 and [O i]), we quantitatively constrain the nature of the innermost region and find that it is distinct from the outer ejecta; the mass of the innermost component is ∼0.03 M ⊙ dominated by Fe (which can initially be 56Ni), expanding with a velocity of ∼760 km s−1. We argue that the nature of the inner component is explained by the failed/weak white-dwarf thermonuclear explosion scenario. We suggest that a fraction of the 56Ni-rich materials initially confined in (the envelope of) the bound remnant can later be ejected by the energy input through the 56Ni/Co/Fe decay, forming the second unbound ejecta component which manifests itself as the inner dense component seen in the late phase.

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Section: Introductionsupporting

confidence: 70%

Section: Introductionmentioning

confidence: 99%

Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core

Maeda

Kawabata

2022

ApJ

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“…Foley et al (2014) speculate about the existence of such a bound remnant in SN 2008ha and suggest that it emits a wind preventing the spectra from transitioning to the nebular phase which is one of the most characterisitc properties of SN Iax spectra. Moreover, evidence for a bound remnant was also found in the slowly declining late-time light curve of SN 2014dt by Kawabata et al (2018) and very recently in SN 2019muj (Kawabata et al 2021). The latter also employ their analytical, phenomenological light curve model to other SNe Iax and conclude that their late-time light curves are well matched assuming radiating burning products at low velocities.…”

Section: Introductionmentioning

confidence: 75%

Type Iax supernovae from deflagrations in Chandrasekhar mass white dwarfs

Lach,

Callan,

Bubeck

et al. 2021

Preprint

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Context. Due to the ever increasing number of observations during the past decades Type Ia supernovae are nowadays regarded as a heterogeneous class of optical transients consisting of several sub-types. One of the largest of these subclasses is the class of Type Iax supernovae. They have been suggested to originate from pure deflagrations in carbon-oxygen Chandrasekhar-mass white dwarfs because the outcome of this explosion scenario is in general agreement with their sub-luminous nature. Aims. Although a few deflagration studies have already been carried out, the full diversity of the class is not captured yet. This, in particular, holds for the faint end of the subclass. We therefore present a parameter study of single-spot ignited deflagrations in Chandrasekhar-mass white dwarfs varying the location of the ignition spark, the central density, the metallicity and the composition of the white dwarf. We also explore a rigidly rotating progenitor to investigate whether the effect of rotation can spawn additional trends. Methods. We carry out three dimensional hydrodynamic simulations employing the leafs code. Subsequently, detailed nucleosynthesis results are obtained with the nuclear network code yann. In order to compare our results to observations we calculate synthetic spectra and light curves with the artis code. Results. The new set of models extends the range in brightness covered by previous studies to the lower end. Our single-spot ignited explosions produce 56 Ni masses from 5.8 × 10 −3 to 9.2 × 10 −2 M . In spite of the wide exploration of the parameter space the main characteristics of the models are primarily driven by the mass of 56 Ni and form a one-dimensional sequence. Secondary parameters seem to have too little impact to explain the observed trend in the faint part of the Type Iax supernova class. We report kick velocities of the gravitationally bound explosion remnants from 6.9 to 369.8 km s −1 . The magnitude as well as the direction of the natal kick is found to depend on the strength of the deflagration. Conclusions. This work corroborates the results of previous studies of deflagrations in Chandrasekhar-mass white dwarfs. The wide exploration of the parameter space in initial conditions and viewing-angle effects in the radiative transfer lead to a significant spread in the synthetic observables. The trends in observational properties towards the faint end of the class are, however, not reproduced. This motivates a quantification of the systematic uncertainties in the modelling procedure and the influence of the 56 Ni -rich bound remnant to get to the bottom of these discrepancies. Moreover, while the pure deflagration scenario remains a favorable explanation for bright and intermediate luminosity Type Iax supernovae, the possibility that this subclass does not consist of only one explosion scenario needs to be taken into account.

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“…For SNe Iax, the lower line velocities suggest that the explosion energies must be lower. The explosion produces less amount of ejecta as compared to SNe Ia and leaves behind a bound remnant (Kawabata et al 2021). The abundance distribution in the ejecta is mixed (Li et al 2003;Branch et al 2004).…”

Section: Introductionmentioning

confidence: 99%

SN 2020sck: deflagration in a carbon-oxygen white dwarf

Dutta,

Sahu,

Anupama

et al. 2021

Preprint

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We present optical U BV RI photometry and low-to-medium resolution spectroscopic observations of type Iax SN 2020sck spanning −5.5 d to +67 d from maximum light in the B-band. From the photometric analysis we find ∆m B (15) = 2.03 ± 0.05 mag and M B = −17.81 ± 0.22 mag. Radiation diffusion model fit to the quasi-bolometric light curve indicates 0.13 ± 0.02 M of 56 Ni and 0.34 M of ejecta are synthesized in the explosion. Comparing the observed quasi-bolometric light curve with angle-averaged bolometric light curve of three-dimensional pure deflagration explosion of M ch carbonoxygen white dwarf, we find agreement with a model in which 0.16 M of 56 Ni and 0.37 M of ejecta is formed. By comparing the +1.4 day spectrum of SN 2020sck with synthetic spectrum generated using SYN++, we find absorption features due to C ii, C iii and O i. These are unburned materials in the explosion and indicate a C-O white dwarf. One dimensional radiative transfer modeling of the spectra with TARDIS shows higher density in the ejecta near the photosphere and a steep decrease in the outer layers with an ejecta composition dominated mostly by C, O, Si, Fe, and Ni. The star formation rate of the host galaxy computed from the luminosity of the Hα (λ6563) line is 0.09 M yr −1 indicating a relatively young stellar environment.

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Intermediate luminosity type Iax supernova 2019muj with narrow absorption lines: Long-lasting radiation associated with a possible bound remnant predicted by the weak deflagration model

Cited by 14 publications

References 67 publications

Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core

Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core

Type Iax supernovae from deflagrations in Chandrasekhar mass white dwarfs

SN 2020sck: deflagration in a carbon-oxygen white dwarf

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