SN 2011fe: A Laboratory for Testing Models of Type Ia Supernovae

Chomiuk, Laura

doi:10.1017/pasa.2013.24

Cited by 18 publications

(20 citation statements)

References 110 publications

(212 reference statements)

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“…While it is similar to SN 2011fe in many respects (e.g., in its color evolution around peak, as well as the apperance of its nebular spectra; see Amanullah et al 2015, but see Marion et al 2015 for a possible early excess of blue light. For more information on SN 2011fe, see, e.g., Li et al 2011;Chomiuk 2013;Kasen & Nugent 2013;Graur et al 2014a), it has a slightly broader light curve. Specifically, by fitting early-time data, Silverman et al (2012) Here, we adopt the value of peak B-band light derived by Munari et al (2013), so that all phases are reported relative to 2012 June 4.5.…”

Section: Discussionmentioning

confidence: 99%

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

Graur

Zurek

Shara

et al. 2016

ApJ

103

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Seitenzahl et al. have predicted that roughly three years after its explosion, the light we receive from a Type Ia supernova (SN Ia) will come mostly from reprocessing of electrons and X-rays emitted by the radioactive decay chain 57 Co→ 57 Fe, instead of positrons from the decay chain 56 Co→ 56 Fe that dominates the SN light at earlier times. Using the Hubble Space Telescope, we followed the light curve of the SN Ia SN 2012cg out to 1055 days after maximum light. Our measurements are consistent with the light curves predicted by the contribution of energy from the reprocessing of electrons and X-rays emitted by the decay of 57 Co, offering evidence that 57 Co is produced in SN Ia explosions. However, the data are also consistent with a light echo ∼14 mag fainter than SN 2012cg at peak. Assuming no light-echo contamination, the mass ratio of 57 Ni and 56 Ni produced by the explosion, a strong constraint on any SN Ia explosion models, is 0.043 0.011 0.012 -+ , roughly twice Solar. In the context of current explosion models, this value favors a progenitor white dwarf with a mass near the Chandrasekhar limit.

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Section: Discussionmentioning

confidence: 99%

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

Graur

Zurek

Shara

et al. 2016

ApJ

103

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“…Being the nearest SN Ia event in 25 years, and having been discovered very early, SN 2011fe was extremely well studied, and has permitted many tests relevant to the progenitor question (see Chomiuk 2013 andKasen & for reviews). SN 2011fe was about as typical as a SN Ia can be, in all of its observed characteristics , making it particularly relevant for addressing the question of the progenitors of SNe Ia, as a population.…”

Section: The Case Of Sn 2011fementioning

confidence: 99%

Observational Clues to the Progenitors of Type Ia Supernovae

Maoz

Mannucci

Nelemans

2014

Annu. Rev. Astron. Astrophys.

954

894

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Type-Ia supernovae (SNe Ia) are important distance indicators, element factories, cosmic-ray accelerators, kinetic-energy sources in galaxy evolution, and endpoints of stellar binary evolution. It has long been clear that a SN Ia must be the runaway thermonuclear explosion of a degenerate carbon-oxygen stellar core, most likely a white dwarf (WD). However, the specific progenitor systems of SNe Ia, and the processes that lead to their ignition, have not been identified. Two broad classes of progenitor binary systems have long been considered: single-degenerate (SD), in which a WD gains mass from a non-degenerate star; and doubledegenerate (DD), involving the merger of two WDs. New theoretical work has enriched these possibilities with some interesting updates and variants. We review the significant recent observational progress in addressing the progenitor problem. We consider clues that have emerged from the observed properties of the various proposed progenitor populations, from studies of their sites -pre-and post-explosion, from analysis of the explosions themselves, and from the measurement of event rates. The recent nearby and well-studied event, SN 2011fe, has been particularly revealing. The observational results are not yet conclusive, and sometimes prone to competing theoretical interpretations. Nevertheless, it appears that DD progenitors, long considered the underdog option, could be behind some, if not all, SNe Ia. We point to some directions that may lead to future progress.

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“…All came up empty handed (see Chomiuk 2013 for an early review, and further developments by Lundqvist et al 2015, Graham et al 2015a, and Taubenberger et al 2015. More details on the implications of our radio limits for the progenitor system can be read in Chomiuk et al (2012b).…”

Section: Sn 2011fementioning

confidence: 99%

A Deep Search for Prompt Radio Emission From Thermonuclear Supernovae With the Very Large Array

Chomiuk

Söderberg

Chevalier

et al. 2016

ApJ

Self Cite

119

179

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Searches for circumstellar material around Type Ia supernovae (SNe Ia) are some of the most powerful tests of the nature of SN Ia progenitors, and radio observations provide a particularly sensitive probe of this material. Here, we report radio observations for SNeIa and their lower-luminosity thermonuclear cousins. We present the largest, most sensitive, and spectroscopically diverse study of prompt (D  t 1 . All observations yield non-detections, placing strong constraints on the presence of circumstellar material. We present analytical models for the temporal and spectral evolution of prompt radio emission from thermonuclear SNe as expected from interaction with either wind-stratified or uniform density media. These models allow us to constrain the progenitor mass loss rates, with limits in the range of --- M 10 10 9 4  M yr −1 , assuming a wind velocity of v w = 100 km s −1 . We compare our radio constraints with measurements of Galactic symbiotic binaries to conclude that 10% of thermonuclear SNe have red giant companions.

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SN 2011fe: A Laboratory for Testing Models of Type Ia Supernovae

Cited by 18 publications

References 110 publications

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

Observational Clues to the Progenitors of Type Ia Supernovae

A Deep Search for Prompt Radio Emission From Thermonuclear Supernovae With the Very Large Array

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SN 2011fe: A Laboratory for Testing Models of Type Ia Supernovae

Cited by 18 publications

References 110 publications

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF 57Co

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF 57Co

Observational Clues to the Progenitors of Type Ia Supernovae

A Deep Search for Prompt Radio Emission From Thermonuclear Supernovae With the Very Large Array

Contact Info

Product

Resources

About

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co

LATE-TIME PHOTOMETRY OF TYPE IA SUPERNOVA SN 2012cg REVEALS THE RADIOACTIVE DECAY OF ⁵⁷Co