EVLA OBSERVATIONS CONSTRAIN THE ENVIRONMENT AND PROGENITOR SYSTEM OF Type Ia SUPERNOVA 2011fe

Chomiuk, Laura; Söderberg, A. M.; Moe, Maxwell; Chevalier, Roger A.; Rupen, M. P.; Badenes, Carles; Margutti, R.; Fransson, Claes; Fong, W.; Dittmann, Jason

doi:10.1088/0004-637x/750/2/164

Cited by 190 publications

(289 citation statements)

References 93 publications

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“…Additionally, SN 2011fe, a SN Ia which exploded in a nearby galaxy, showed no evidence of interaction with circumstellar material at radio, X-ray, and optical wavelengths (e.g. Margutti et al 2012;Chomiuk et al 2012;Patat et al 2013), and pre-explosion images exclude most types of donor stars of the SD channel (Li et al 2011a). A&A 563, A83 (2014) These difficulties in reconciling the observational evidence with the predictions of the SD channel are avoided in the DD channel, but this channel has its own difficulties.…”

Section: Introductionmentioning

confidence: 99%

Theoretical uncertainties of the Type Ia supernova rate

Claeys

Pols

Izzard

et al. 2014

A&A

280

326

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It is thought that Type Ia supernovae (SNe Ia) are explosions of carbon-oxygen white dwarfs (CO WDs). Two main evolutionary channels are proposed for the WD to reach the critical density required for a thermonuclear explosion: the single degenerate (SD) scenario, in which a CO WD accretes from a non-degenerate companion, and the double degenerate (DD) scenario, in which two CO WDs merge. However, it remains difficult to reproduce the observed SN Ia rate with these two scenarios. With a binary population synthesis code we study the main evolutionary channels that lead to SNe Ia and we calculate the SN Ia rates and the associated delay-time distributions. We find that the DD channel is the dominant formation channel for the longest delay times. The SD channel with helium-rich donors is the dominant channel at the shortest delay times. Our standard model rate is a factor of five lower than the observed rate in galaxy clusters. We investigate the influence of ill-constrained aspects of single-and binary-star evolution and uncertain initial binary distributions on the rate of Type Ia SNe. These distributions, as well as uncertainties in both helium star evolution and common envelope evolution, have the greatest influence on our calculated rates. Inefficient common envelope evolution increases the relative number of SD explosions such that for α ce = 0.2 they dominate the SN Ia rate. Our highest rate is a factor of three less than the galaxy-cluster SN Ia rate, but compatible with the rate determined in a field-galaxy dominated sample. If we assume unlimited accretion onto WDs, to maximize the number of SD explosions, our rate is compatible with the observed galaxy-cluster rate.

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Section: Introductionmentioning

confidence: 99%

Theoretical uncertainties of the Type Ia supernova rate

Claeys

Pols

Izzard

et al. 2014

A&A

280

326

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“…This has been suggested to be evidence that supports the SD scenario because such CSM is generally expected to exist around SN Ia progenitor as the result of mass transfer from the companion star, as well as from WD winds. On the other hand, there is some evidence in favour of the DD scenario, e.g., the nondetection of pre-explosion companion stars in normal SNe Ia (Li et al 2011;Bloom et al 2012), the absence of H/He features in the nebular spectra of SNe Ia (Leonard 2007;Lundqvist et al 2013Lundqvist et al , 2015Shappee, Kochanek & Stanek 2013;Maguire et al 2016), the lack of radio and X-ray emission around peak brightness (Bloom et al 2012;Brown et al 2012;Chomiuk et al 2012;Horesh et al 2012;Margutti et al 2014), and the absence of a sur-viving companion star in SN Ia remnants (Kerzendorf et al 2009;Schaefer & Pagnotta 2012).…”

Section: Introductionmentioning

confidence: 99%

Constraining the progenitor of the Type Ia Supernova SN 2012cg

Liu

Stancliffe

2016

Mon. Not. R. Astron. Soc.

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The nature of the progenitors of Type Ia supernovae (SNe Ia) is not yet fully understood. In the single-degenerate (SD) scenario, the collision of the SN ejecta with its companion star is expected to produce detectable ultraviolet (UV) emission in the first few days after the SN explosion within certain viewing angles. It was recently found that the B − V colour of the nearby SN Ia SN 2012cg at about sixteen days before the maximum B-band brightness was about 0.2 mag bluer than those of other normal SNe Ia, which was reported as the first evidence for excess blue light from the interaction of normal SN Ia ejecta with its companion star. In this work, we compare current observations for SN 2012cg from its pre-explosion phase to the late-time nebular phase with theoretical predictions from binary evolution and population synthesis calculations for a variety of popular progenitor scenarios. We find that a main-sequence donor or a carbon-oxygen white dwarf donor binary system is more likely to be the progenitor of SN 2012cg. However, both scenarios also predict properties which are in contradiction to the observed features of this system. Taking both theoretical and observational uncertainties into account, we suggest that it might be too early to conclude that SN 2012cg was produced from an explosion of a Chandrasekhar-mass white dwarf in the SD scenario. Future observations and improved detailed theoretical modelling are still required to place a more stringent constraint on the progenitor of SN 2012cg.

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“…Using more recent radio observations, Chomiuk et al (2011) analyzed EVLA observations of early SN Ia spectra. From their non-detections, they found typical upper limitsṀ/u w 10 −7 M yr −1 /(100 km s −1 ) for most sources (private communication).…”

Section: Upper Limitsmentioning

confidence: 99%

“…From their non-detections, they found typical upper limitsṀ/u w 10 −7 M yr −1 /(100 km s −1 ) for most sources (private communication). Chomiuk et al (2012) reported upper limits ofṀ/u w = (6 × 10 −10 −3 × 10 −9 ) M /yr/(100 km s −1 ) for non-detections of radio emission from SN2011fe, the closest SN Ia in 25 years. For the lower wind speed used in our model, the upper limits are correspondingly lower, hence the upper limit of the wind mass-loss rate of the donor becomes 10 −8 M yr −1 for typical SD SN Ia progenitors, and (6 × 10 −11 −3 × 10 −10 ) M /yr for SN2011fe.…”

Section: Upper Limitsmentioning

confidence: 99%

Obscuration of supersoft X-ray sources by circumbinary material

Nielsen

Dominik

Nelemans

et al. 2012

A&A

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Context. The progenitors of Type Ia supernovae are usually assumed to be either a single white dwarf accreting from a non-degenerate companion (the single-degenerate channel) or the result of two merging white dwarfs (the double degenerate channel). However, no consensus currently exists as to which progenitor scenario is the correct one, or whether the observed Type Ia supernovae rate is produced by a combination of both channels. Unlike a double degenerate progenitor, a single-degenerate progenitor is expected to emit supersoft X-rays for a prolonged period of time (∼1 Myr) as a result of the burning of accreted matter on the surface of the white dwarf. An argument against the single-degenerate channel as a significant producer of Type Ia supernovae has been the lack of observed supersoft X-ray sources and the lower-than-expected integrated soft X-ray flux from elliptical galaxies. Aims. We wish to determine whether it is possible to obscure the supersoft X-ray emission from a nuclear-burning white dwarf in an accreting single-degenerate binary system. In the case of obscured systems we wish to determine their general observational characteristics. Methods. We examine the emergent X-ray emission from a canonical supersoft X-ray system surrounded by a spherically symmetric configuration of material, assuming a black-body spectrum with T bb = 50 eV and L = 10 38 erg s −1 . The circumbinary material is assumed to be of solar chemical abundances, and we leave the mechanism behind the mass-loss into the circumbinary region unspecified. Results. We find that relatively low circumstellar mass-loss rates,Ṁ = 10 −9 −10 −8 M yr −1 , at binary separations of ∼1 AU or less, will cause significant attenuation of the X-rays from the supersoft X-ray source. These circumstellar mass-loss rates are sufficient to make a canonical supersoft X-ray source in typical external galaxies unobservable in Chandra. Conclusions. If steadily accreting, nuclear-burning white dwarfs are canonical supersoft X-ray sources our analysis suggests that they can be obscured by relatively modest circumbinary mass-loss rates. This may explain the discrepancy of supersoft sources relative to the Type Ia supernova rate inferred from observations if the single-degenerate progenitor scenario contributes significantly to the Type Ia supernova rate. Recycled emissions from obscured systems may be visible in wavebands other than X-rays. It may also explain the lack of observed supersoft sources in symbiotic binary systems.

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EVLA OBSERVATIONS CONSTRAIN THE ENVIRONMENT AND PROGENITOR SYSTEM OF Type Ia SUPERNOVA 2011fe

Cited by 190 publications

References 93 publications

Theoretical uncertainties of the Type Ia supernova rate

Theoretical uncertainties of the Type Ia supernova rate

Constraining the progenitor of the Type Ia Supernova SN 2012cg

Obscuration of supersoft X-ray sources by circumbinary material

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