A hyper-runaway white dwarf in Gaia DR2 as a Type Iax supernova primary remnant candidate

Ruffini, Nicholas; Casey, Andrew R.

doi:10.1093/mnras/stz2176

Cited by 11 publications

(5 citation statements)

References 78 publications

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“…Given our constraints on the relative rates of SNe Iax, this would imply 3 − 25 Iax SNRs in our Galaxy. In the CONe WD + He star channel for SNe Iax, in addition to the partially burnt bound remnant or primary remnant (PR), the kicked companion or donor remnant (DR), that may have evolved to the WD stage, is also expected to survive (Ruffini & Casey 2019). In principle, both PRs and DRs could be detectable in the Galaxy, although SN Ia remnants may be more difficult to detect compared to CCSN remnants (Sarbadhicary et al 2017).…”

Section: Discussionmentioning

confidence: 99%

SN 2020kyg and the rates of faint Iax Supernovae from ATLAS

Srivastav,

Smartt,

Huber

et al. 2021

Preprint

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We present multi-wavelength follow-up observations of the ATLAS discovered faint Iax supernova SN 2020kyg (ATLAS20nuc) discovered in NGC 5012 at ∼ 40 Mpc. SN 2020kyg peaked at an absolute magnitude of 𝑀 𝑔 ≈ −14.9 ± 0.2, making it another member of the faint Iax supernova population. The bolometric light curve is adequately fit with an Arnett model, requiring only ≈ 7 × 10 −3 M of radioactive 56 Ni, with an ejected mass of 𝑀 ej ∼ 0.4 M . The 𝑔-band rise time inferred from the fit is ∼ 10 days, consistent with the low luminosity. The photospheric velocity around maximum, deduced from Si 𝜆6355 is ∼ 4500 km s −1 implying a low kinetic energy of 𝐸 51 ≈ 0.05 ± 0.02 erg. A self-consistent model constructed using the 1D radiative transfer code for the early optical spectra is dominated by carbon, oxygen, neon and intermediate mass elements like silicon, sulphur and magnesium. The model deviates significantly from the observed spectrum at > +14 days, suggesting the ejecta is transitioning towards an optically thin state, and/or presence of significant radioactive material in the outer layers of the ejecta. In order to constrain the rates of SNe Iax in the local Universe, we construct a homogeneous volume-limited sample of 902 transients observed by ATLAS within 100 Mpc during a 3.5 year span. Using this sample, we constrain the rates of faint Iax (𝑀 𝑟 −16) events within 60 Mpc at 12 +13 −8 % of the SN Ia rate. The overall Iax rate, at 15 +15 −9 % of the Ia rate, is dominated by the low-luminosity events, with luminous SNe Iax (𝑀 𝑟 −17.5) like 2002cx and 2005hk accounting for less than 1% of the Ia rate. We favor the hybrid CONe WD + He star progenitor channel involving a failed deflagration of a near Chandrasekhar mass white dwarf, expected to leave a bound remnant and a surviving secondary companion, as a candidate explanation for faint Iax explosions. This scenario requires short delay times, consistent with the observed environments of SNe Iax. Furthermore, binary population synthesis calculations have suggested rates of 1 − 18% of the SN Ia rate for this channel, consistent with our rate estimates.

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Section: Discussionmentioning

confidence: 99%

SN 2020kyg and the rates of faint Iax Supernovae from ATLAS

Srivastav,

Smartt,

Huber

et al. 2021

Preprint

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“…If these massive DQs formed in a double degenerate merger, this would provide the necessary delay to make these stars appear younger than they really are. One star where we clearly see a discrepancy between the total age assuming single star evolution and the age based on kinematics is LP 93-21, which is a massive DQ with halo like orbit (Kawka et al 2020) and is thus highly unlikely to be the unburnt remnant of a subluminous Type Ia supernova explosion (e.g., Vennes et al 2017) as proposed by Ruffini & Casey (2019). It is likely that the majority of these cooler massive DQs will also harbour a magnetic field and be fast rotators.…”

Section: Hot Dq White Dwarfsmentioning

confidence: 82%

Clues to the origin and properties of magnetic white dwarfs

Kawka

2019

Proc. IAU

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A significant fraction of white dwarfs possess a magnetic field with strengths ranging from a few kG up to about 1000 MG. However, the incidence of magnetism varies when the white dwarf population is broken down into different spectral types providing clues on the formation of magnetic fields in white dwarfs. Several scenarios for the origin of magnetic fields have been proposed from a fossil field origin to dynamo generation at various stages of evolution. Offset dipoles are often assumed sufficient to model the field structure, however time-resolved spectropolarimetric observations have revealed more complex structures such as magnetic spots or multipoles. Surface mapping of these field structures combined with measured rotation rates help distinguish scenarios involving single star evolution from other scenarios involving binary interactions. I describe key observational properties of magnetic white dwarfs such as age, mass, and field strength, and confront proposed formation scenarios with these properties.

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“…Vennes et al (2017) interpreted LP 40-365 as a partly burnt WD remnant due to its high proper motion and peculiar atmosphere that is dominated by IMEs (see also Raddi et al 2018Raddi et al , 2019Hermes et al 2021). Ruffini & Casey (2019) suggested that a hyper-runaway WD in Gaia DR2, LP 93-21, could be another candidate for such events. Foley et al (2014) reported a post-explosion detection of a thermally pulsing AGB-like source at the position of SN 2008ha by using HST images obtained 4.1 yr after the explosion.…”

Section: Searches For Surviving Wd Remnantsmentioning

confidence: 99%

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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A hyper-runaway white dwarf in Gaia DR2 as a Type Iax supernova primary remnant candidate

Cited by 11 publications

References 78 publications

SN 2020kyg and the rates of faint Iax Supernovae from ATLAS

SN 2020kyg and the rates of faint Iax Supernovae from ATLAS

Clues to the origin and properties of magnetic white dwarfs

Type Ia Supernova Explosions in Binary Systems: A Review

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