Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae

Liu, W.-M.; Chen, Wen-Cong; Wang, Bo; Han, Zhanwen

doi:10.1051/0004-6361/201014180

Cited by 35 publications

(22 citation statements)

References 76 publications

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“…In single-degenerate (SD) progenitor models for SNe Ia, we expect the SN to sweep up material ablated from a close companion star and/or in the circumstellar environment. This material should emit and be detectable in late-time spectra as narrow emission lines (Marietta et al 2000;Mattila et al 2005;Liu et al 2010Liu et al , 2012Liu et al , 2013aPan et al 2012;Lundqvist et al 2013 Upon visual inspection of all late-time SN Iax spectra, we find no obvious hydrogen or helium narrow-line emission. As in Lundqvist et al (2015), we also examine each latetime spectra for Ca ii and O i emission but find no visual detections.…”

Section: Search For Late-time Emission Featuresmentioning

confidence: 76%

Detection of circumstellar helium in Type Iax progenitor systems

Jacobson-Galán

Foley

Schwab

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present direct spectroscopic modeling of 44 Type Iax supernovae (SNe Iax) using spectral synthesis code SYNAPPS. We confirm detections of helium emission in the earlytime spectra of two SNe Iax: SNe 2004cs and 2007J. These He i features are better fit by a pure-emission Gaussian than by a P-Cygni profile, indicating that the helium emission originates from the circumstellar environment rather than the SN ejecta. Based on the modeling of the remaining 42 SNe Iax, we find no obvious helium features in other SN Iax spectra. However, ≈ 76% of our sample lack sufficiently deep luminosity limits to detect helium emission with a luminosity of that seen in SNe 2004cs and 2007J. Using the objects with constraining luminosity limits, we calculate that 33% of SNe Iax have detectable helium in their spectra. We examine 11 SNe Iax with late-time spectra and find no hydrogen or helium emission from swept up material. For latetime spectra, we calculate typical upper limits of stripped hydrogen and helium to be 2×10 −3 M and 10 −2 M , respectively. While detections of helium in SNe Iax support a white dwarf-He star binary progenitor system (i.e., a single-degenerate [SD] channel), non-detections may be explained by variations in the explosion and ejecta material. The lack of helium in the majority of our sample demonstrates the complexity of SN Iax progenitor systems and the need for further modeling. With strong independent evidence indicating that SNe Iax arise from a SD channel, we caution the common interpretation that the lack of helium or hydrogen emission at late-time in SN Ia spectra rules out SD progenitor scenarios for this class. (UCSC) (Jha 2017), all spectroscopically similar to the prototypical SN Iax, SN 2002cx (Li et al. 2003. As is the case for SNe Ia, the progenitor system and explosion mechanisms of SNe Iax are still unclear. Due to their spectroscopic agreement with SNe Ia near maximum light, SNe Iax are generally considered to be thermonuclear explosions that result from a white dwarf (WD) in a binary system. Based on stellar population estimates (Foley et al. 2009; McCully et al. 2014), SNe Iax are found

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Section: Search For Late-time Emission Featuresmentioning

confidence: 76%

Detection of circumstellar helium in Type Iax progenitor systems

Jacobson-Galán

Foley

Schwab

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…This has been observed in several binary population synthesis studies (Ruiter et al 2009(Ruiter et al , 2011Wang et al 2009b,a;Meng & Yang 2010;Piersanti et al 2014;Liu et al 2015). Liu et al (2010) present a model (originally intended to explain a different kind of system) that begins with a 7 M + 4 M binary system that undergoes two phases of mass transfer and common envelope evolution, before resulting in a 1 M C/O WD + 2 M He star. As the He star evolves, it again fills its Roche lobe and begins stable mass transfer onto the white dwarf that could lead to the SN Iax.…”

Section: Thus the Divergent Metallicity Distributions Of Sne Iax Andmentioning

confidence: 81%

Constraining Type Iax supernova progenitor systems with stellar population age dating

Takaro

Foley

McCully

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Type Iax supernovae (SNe Iax) are the most common class of peculiar SNe. While they are thought to be thermonuclear white-dwarf (WD) SNe, SNe Iax are observationally similar to, but distinct from SNe Ia. Unlike SNe Ia, where roughly 30% occur in early-type galaxies, only one SN Iax has been discovered in an early-type galaxy, suggesting a relatively short delay time and a distinct progenitor system. Furthermore, one SN Iax progenitor system has been detected in pre-explosion images with its properties consistent with either of two models: a short-lived (<100 Myr) progenitor system consisting of a WD primary and a He-star companion, or a singular Wolf-Rayet progenitor star. Using deep Hubble Space Telescope images of nine nearby SN Iax host galaxies, we measure the properties of stars within 200 pc of the SN position. The ages of local stars, some of which formed with the SN progenitor system, can constrain the time between star formation and SN, known as the delay time. We compare the local stellar properties to synthetic photometry of single-stellar populations, fitting to a range of possible delay times for each SN. With this sample, we uniquely constrain the delay-time distribution for SNe Iax, with a median and 1 − σ confidence interval delay time of 63 +58 −15 × 10 6 years. The measured delay-time distribution provides an excellent constraint on the progenitor system for the class, indicating a preference for a WD progenitor system over a Wolf-Rayet progenitor star.

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“…The late-time HST WFC3 photometry from Graur et al (2015) is also consistent with this model. The pre-explosion limits suggest that the progenitor system of SN2012cg did not have a helium star donor (e.g., Wang et al 2014;Liu et al 2010).…”

Section: Discussionmentioning

confidence: 99%

SN 2012cg: EVIDENCE FOR INTERACTION BETWEEN A NORMAL SN Ia AND A NON-DEGENERATE BINARY COMPANION

Marion

Brown

Vinkó

et al. 2016

ApJ

156

202

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We report evidence for excess blue light from the Type Ia supernova (Sn Ia) SN2012cg at 15 and 16 days before maximum B-band brightness. The emission is consistent with predictions for the impact of the supernova on a nondegenerate binary companion. This is the first evidence for emission from a companion to a normal SNIa. Sixteen days before maximum light, the B V -color of SN2012cg is 0.2 mag bluer than for other normal SNIa. At later times, this supernova has a typical SNIa light curve, with extinction-corrected M 19.62 0.02 B = - mag and m B 0.86 0.02 15 ( ) D =  . Our data set is extensive, with photometry in seven filters from five independent sources. Early spectra also show the effects of blue light, and high-velocity features are observed at early times. Near maximum, the spectra are normal with a silicon velocity v Si =−10,500 km s −1 . Comparing the early data with models by Kasen favors a main-sequence companion of about six solar masses. It is possible that many other SN Ia have main-sequence companions that have eluded detection because the emission from the impact is fleeting and faint.

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Helium-star evolutionary channel to super-Chandrasekhar mass type Ia supernovae

Cited by 35 publications

References 76 publications

Detection of circumstellar helium in Type Iax progenitor systems

Detection of circumstellar helium in Type Iax progenitor systems

Constraining Type Iax supernova progenitor systems with stellar population age dating

SN 2012cg: EVIDENCE FOR INTERACTION BETWEEN A NORMAL SN Ia AND A NON-DEGENERATE BINARY COMPANION

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