Sub-Chandrasekhar-mass detonations are in tension with the observed t0−MNi56 relation of type Ia supernovae

Kushnir, Doron; Wygoda, Nahliel; Sharon, Amir

doi:10.1093/mnras/staa3017

Cited by 23 publications

(36 citation statements)

References 73 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The converging detonation waves trigger a second detonation at the carbon-oxygen core, hence producing a prompt eruption (Moll et al 2014;Raskin et al 2014;Tanikawa et al 2019;Gronow et al 2020). While some observational results seem to favor the double-degenerate scenario (Woosley & Kasen 2011;Maoz et al 2014;Glasner et al 2018), suggesting that they might constitute the majority population of thermonuclear supernovae (Flörs et al 2019;Cheng et al 2020;Li et al 2021), some recent studies found that they could be in a tight tension with the γ-ray ejected time against nickel-mass relation (Kushnir et al 2020).…”

Section: Appendix a Accuracy Of Linear Interpolationmentioning

confidence: 99%

Delayed Detonation Thermonuclear Supernovae with an Extended Dark Matter Component

Chan

Chu

Leung

et al. 2021

ApJ

View full text Add to dashboard Cite

We present spherically symmetric simulations of the thermonuclear explosion of a white dwarf admixed with an extended component of fermionic dark matter, using the deflagration model with the deflagration-detonation transition. In all the dark matter admixed models we have considered, the dark matter is left behind after the explosion as a compact dark star. The presence of dark matter lengthens the deflagration phase to produce a similar amount of iron-group elements and more thermoneutrinos. Dark matter admixed models also give dimmer but slowly declining light curves, consistent with some observed peculiar supernovae. Our results suggest a formation path for dark compact objects that mimic sub-solar-mass black holes as dark gravitational sources.Unified Astronomy Thesaurus concepts: Dark matter (353); Type Ia supernovae (1728); Hydrodynamical simulations (767); Supernova neutrinos (1666); Light curves (918) The Deflagration-Detonation Transition (DDT) as a Supernova Explosion ModelWDs are believed to be the progenitors for thermonuclear supernovae (Hillebrandt et al. 2013;Maoz et al. 2014;Livio & Mazzali 2018). However, it is not clear which kind of WDs and explosion mechanisms are responsible for such energetic events (Ruiter 2019). It is believed that most of the progenitor

show abstract

Section: Appendix a Accuracy Of Linear Interpolationmentioning

confidence: 99%

Delayed Detonation Thermonuclear Supernovae with an Extended Dark Matter Component

Chan

Chu

Leung

et al. 2021

ApJ

View full text Add to dashboard Cite

show abstract

“…Here, 〈Σ〉 Ni56 is the column density of the ejecta Ni 56 and κ eff is the effective opacity ( ≈ 0.025 cm 2 g −1 for 56 Co; Swartz et al 1995;Jeffery 1999;Kushnir et al 2020). In a homologous expansion, 〈Σ〉 Ni56 t 2 is constant.…”

Section: The Fast Radioactive Shell Scenariomentioning

confidence: 99%

AT 2018lqh and the Nature of the Emerging Population of Day-scale Duration Optical Transients

Ofek

Adams

Waxman

et al. 2021

ApJ

View full text Add to dashboard Cite

We report on the discovery of AT 2018lqh (ZTF 18abfzgpl)—a rapidly evolving extragalactic transient in a star-forming host at 242 Mpc. The transient g-band light curve’s duration above a half-maximum light is about 2.1 days, where 0.4/1.7 days are spent on the rise/decay, respectively. The estimated bolometric light curve of this object peaked at about 7 × 1042erg s−1—roughly 7 times brighter than the neutron star (NS)–NS merger event AT 2017gfo. We show that this event can be explained by an explosion with a fast (v ∼ 0.08 c) low-mass (≈0.07 M ⊙) ejecta, composed mostly of radioactive elements. For example, ejecta dominated by 56Ni with a timescale of t 0 ≅ 1.6 days for the ejecta to become optically thin for γ-rays fits the data well. Such a scenario requires burning at densities that are typically found in the envelopes of neutron stars or the cores of white dwarfs. A combination of circumstellar material (CSM) interaction power at early times and shock cooling at late times is consistent with the photometric observations, but the observed spectrum of the event may pose some challenges for this scenario. We argue that the observations are not consistent with a shock breakout from a stellar envelope, while a model involving a low-mass ejecta ramming into low-mass CSM cannot explain both the early- and late-time observations.

show abstract

“…Once luminosities are corrected, we determine the amount 56 Ni from the relation log 10 (𝑀 Ni ) = −0.4(𝑀 𝐵 + 19.841 ∓ 0.020) (Scalzo et al 2014, eq. 2), and the WD masses from the fitting relation 𝑀 wd = (0.796 ± 0.008) + 0.383𝑀 Ni (Kushnir et al 2020) which assumes pure detonations, in agreement with Steigerwald & Tejeda (2021). Once we have the SN Ia explosion masses, we determine the PBH mass scale according to Steigerwald & Tejeda (2021) assuming the WD mass function of Kilic et al (2020).…”

Section: Discussionmentioning

confidence: 99%

Type Ia Supernova Magnitude Step from the local Dark Matter Environment

Steigerwald,

Rodrigues,

Profumo

et al. 2021

Preprint

View full text Add to dashboard Cite

Residuals in the Hubble diagram at optical wavelengths and host galaxy stellar mass are observed to correlate in Type Ia supernovae (SNe Ia) ('magnitude step'). Among possible progenitor channels for the associated explosions, those based on dark matter (DM) have attracted significant attention, including our recent proposal that 'normal' SNe Ia from bare detonations in sub-Chandrasekhar white dwarf stars are triggered by the passage of asteroid-mass primordial black holes (PBHs): the magnitude step could then originate from a brightness dependence on stellar properties, on DM properties, or both. Here, we present a method to estimate the local DM density and velocity dispersion of the environment of SN Ia progenitors. We find a luminosity step of 0.52 ± 0.11 mag corresponding to bins of high vs low DM density in a sample of 222 low-redshift events from the Open Supernova Catalog. We investigate whether the magnitude step can be attributed to local DM properties alone, assuming asteroid-mass PBHs. Given the inverse correlation between SN Ia brightness and PBH mass, an intriguing explanation is a spatially-inhomogeneous PBH mass function. If so, a strong mass segregation in the DM density-dependent PBH mass scale is needed to explain the magnitude step. While mass segregation is observed in dense clusters, it is unlikely to be realized on galactic scales. Therefore, if DM consists of asteroid-mass PBHs, the magnitude step is more likely to exist, and dominantly to be attributed to local stellar properties.

show abstract

Sub-Chandrasekhar-mass detonations are in tension with the observed t0−MNi56 relation of type Ia supernovae

Cited by 23 publications

References 73 publications

Delayed Detonation Thermonuclear Supernovae with an Extended Dark Matter Component

Delayed Detonation Thermonuclear Supernovae with an Extended Dark Matter Component

AT 2018lqh and the Nature of the Emerging Population of Day-scale Duration Optical Transients

Type Ia Supernova Magnitude Step from the local Dark Matter Environment

Contact Info

Product

Resources

About