Type Ia Supernovae

Maguire, Kate

doi:10.1007/978-3-319-20794-0_36-1

Cited by 8 publications

(5 citation statements)

References 88 publications

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“…Material from a hydrogen-or helium-rich companion star has been predicted to be stripped (or ablated) during the explosion and result in the presence of low-velocity hydrogen-or helium-rich material in the SN ejecta where it can be energized by the radioactive decay and become visible. Searches for this material have been made in many nearby SN Ia using late-time spectra, without detection 29,[75][76][77][78][79][80][81][82][83][84] . This suggests that either the material is present and is not visible because it is not located cospatially with the radioactive material or that these objects do not have hydrogen-or helium-rich companions.…”

Section: Type Ia Supernovaementioning

confidence: 99%

Observational properties of thermonuclear supernovae

2019

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The explosive death of a star as a supernova is one of the most dramatic events in the Universe. Supernovae have an outsized impact on many areas of astrophysics: they are major contributors to the chemical enrichment of the cosmos and significantly influence the formation of subsequent generations of stars and the evolution of galaxies. Here we review the observational properties of thermonuclear supernovae, exploding white dwarf stars resulting from the stellar evolution of low-mass stars in close binary systems. The best known objects in this class are type Ia supernovae (SN Ia), astrophysically important in their application as standardisable candles to measure cosmological distances and the primary source of iron group elements in the Universe. Surprisingly, given their prominent role, SN Ia progenitor systems and explosion mechanisms are not fully understood; the observations we describe here provide constraints on models, not always in consistent ways. Recent advances in supernova discovery and follow-up have shown that the class of thermonuclear supernovae includes more than just SN Ia, and we characterise that diversity in this review.The modern classification scheme for supernovae traces back to Minkowski 1 who in 1941 split "Type I" from "Type II" supernovae based on optical spectra. Further subdivision of these basic classes has continued on an empirical basis 2, 3 , and in our review we describe the observational properties of what are now called SN Ia, along with other similar objects. The observational classification effort arises from a desire for physical understanding of these objects, explaining our use of the term thermonuclear supernovae in the title. That categorisation is based on the explosion mechanism: objects where the energy released in the explosion is primarily the result of thermonuclear fusion. Given our current state of knowledge, we could equally well call this a review of the observational properties of white dwarf supernovae, a categorisation based on the kind of object that explodes. This is contrasted with core-collapse or massive star supernovae, respectively, in the explosion mechanism or exploding object categorisations. Unlike those objects, where clear observational evidence exists for massive star progenitors and corecollapse (from both neutrino emission and remnant pulsars), the direct evidence for thermonuclear supernova explosions of white dwarfs is limited 4, 5 and not necessarily simply interpretable 6, 7 . Nevertheless, the indirect evidence is strong, though many open questions about the progenitor systems and explosion mechanisms remain.SN Ia are important both to the evolution of the Universe and to our understanding of it. As standardisable candles whose distance can be observationally inferred 8 , SN Ia have a starring role in the discovery of the accelerating expansion of the Universe 9, 10 and in measurement of its current expansion rate 11 . SN Ia are also major contributors to the chemical enrichment of the Universe, producing most of its iron 12 and elem...

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Section: Type Ia Supernovaementioning

confidence: 99%

Observational properties of thermonuclear supernovae

2019

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“…This indicates either the limit to which SNe Ia are standardisable, or that there are further brightness correlations that cannot be uncovered with the size and quality of current samples. This latter possibility could arise from astrophysical uncertainties in the SN Ia progenitor mechanisms, explosion physics, and/or environment (Maoz et al 2014;Maguire 2017;Livio & Mazzali 2018).…”

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The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

Kelsey

Sullivan

Smith

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Analyses of Type Ia supernovae (SNe Ia) have found puzzling correlations between their standardized luminosities and host galaxy properties: SNe Ia in high-mass, passive hosts appear brighter than those in lower mass, star-forming hosts. We examine the host galaxies of SNe Ia in the Dark Energy Survey 3-yr spectroscopically confirmed cosmological sample, obtaining photometry in a series of ‘local’ apertures centred on the SN, and for the global host galaxy. We study the differences in these host galaxy properties, such as stellar mass and rest-frame U − R colours, and their correlations with SN Ia parameters including Hubble residuals. We find all Hubble residual steps to be >3σ in significance, both for splitting at the traditional environmental property sample median and for the step of maximum significance. For stellar mass, we find a maximal local step of 0.098 ± 0.018 mag; ∼0.03 mag greater than the largest global stellar mass step in our sample (0.070 ± 0.017 mag). When splitting at the sample median, differences between local and global U − R steps are small, both ∼0.08 mag, but are more significant than the global stellar mass step (0.057 ± 0.017 mag). We split the data into sub-samples based on SN Ia light-curve parameters: stretch (x1) and colour (c), finding that redder objects (c > 0) have larger Hubble residual steps, for both stellar mass and U − R, for both local and global measurements, of ∼0.14 mag. Additionally, the bluer (star-forming) local environments host a more homogeneous SN Ia sample, with local U − R rms scatter as low as 0.084 ± 0.017 mag for blue (c < 0) SNe Ia in locally blue U − R environments.

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“…Given the enormous effort that has gone into explaining normal SN Ia, it is astounding to think that we may have a better understanding of their peculiar cousins, SN Iax. The Extremes of Thermonuclear Supernovae (Taubenberger 2016) Type Ia Supernovae (Maguire 2016) Unusual Supernovae and Alternative Power Sources (Kasen 2017)…”

Section: Discussionmentioning

confidence: 99%

Handbook of Supernovae

Alsabti¹

2016

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Type Iax supernovae (SN Iax), also called SN 2002cx-like supernovae, are the largest class of "peculiar" white dwarf (thermonuclear) supernovae, with over fifty members known. SN Iax have lower ejecta velocity and lower luminosities, and these parameters span a much wider range, than normal type Ia supernovae (SN Ia). SN Iax are spectroscopically similar to some SN Ia near maximum light, but are unique among all supernovae in their late-time spectra, which never become fully "nebular". SN Iax overwhelmingly occur in late-type host galaxies, implying a relatively young population. The SN Iax 2012Z is the only white dwarf supernova for which a pre-explosion progenitor system has been detected. A variety of models have been proposed, but one leading scenario has emerged: a type Iax supernova may be a pure-deflagration explosion of a carbon-oxygen (or hybrid carbon-oxygen-neon) white dwarf, triggered by helium accretion to the Chandrasekhar mass, that does not necessarily fully disrupt the star.

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Type Ia Supernovae

Cited by 8 publications

References 88 publications

Observational properties of thermonuclear supernovae

Observational properties of thermonuclear supernovae

The effect of environment on Type Ia supernovae in the Dark Energy Survey three-year cosmological sample

Handbook of Supernovae

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