EVOLVING TO TYPE Ia SUPERNOVAE WITH SHORT DELAY TIMES

Wang, Bo; Chen, Xuefei; Meng, Xiangcun; Han, Zhanwen

doi:10.1088/0004-637x/701/2/1540

Cited by 96 publications

(135 citation statements)

References 80 publications

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“…In the He double-detonation model, if the mass-accretion rate is higher than 4 × 10 −8 M yr −1 , the WD can increase its mass (Woosley et al 1986;Wang et al 2009a). However, for low mass-accretion rates (1 × 10 −9 M yr −1 |Ṁ 2 | 4 × 10 −8 M yr −1 ), compressional heating at the base of the accreted He layer plays no significant role, and a layer of unburned He can be accumulated on the surface of the WD.…”

Section: Binary Evolution Calculationsmentioning

confidence: 99%

A progenitor binary and an ejected mass donor remnant of faint type Ia supernovae

Geier

Marsh

Wang

et al. 2013

A&A

116

159

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Type Ia supernovae (SN Ia) are the most important standard candles for measuring the expansion history of the universe. The thermonuclear explosion of a white dwarf can explain their observed properties, but neither the progenitor systems nor any stellar remnants have been conclusively identified. Underluminous SN Ia have been proposed to originate from a so-called double-detonation of a white dwarf. After a critical amount of helium is deposited on the surface through accretion from a close companion, the helium is ignited causing a detonation wave that triggers the explosion of the white dwarf itself. We have discovered both shallow transits and eclipses in the tight binary system CD-30 • 11223 composed of a carbon/oxygen white dwarf and a hot helium star, allowing us to determine its component masses and fundamental parameters. In the future the system will transfer mass from the helium star to the white dwarf. Modelling this process we find that the detonation in the accreted helium layer is sufficiently strong to trigger the explosion of the core. The helium star will then be ejected at such high velocity that it will escape the Galaxy. The predicted properties of this remnant are an excellent match to the so-called hypervelocity star US 708, a hot, helium-rich star moving at more than 750 km s −1 , sufficient for it to leave the Galaxy. The identification of both progenitor and remnant provides a consistent picture of the formation and evolution of underluminous SNIa.

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Section: Binary Evolution Calculationsmentioning

confidence: 99%

A progenitor binary and an ejected mass donor remnant of faint type Ia supernovae

Geier

Marsh

Wang

et al. 2013

A&A

116

159

View full text Add to dashboard Cite

show abstract

“…In addition, another two channels such as the early asymptotic giant branch channel and the thermal-pulsing asymptoticgiant branch channel can also produce CO WD + He star systems (Wang et al 2009b). Employing Hurley's rapid BSE code, Wang et al (2009b) investigated the initial parameter distribution of WD + He star systems.…”

Section: Formation Of Wd + He Star Systemsmentioning

confidence: 99%

“…Employing Hurley's rapid BSE code, Wang et al (2009b) investigated the initial parameter distribution of WD + He star systems. Their simulated results show that the initial mass of the CO WDs is in the range of 0.85-1.2 M 2 , and the initial mass of the He stars is in the range of 1.0-2.8 M , which depends on the common-envelope parameters α CE λ.…”

Section: Formation Of Wd + He Star Systemsmentioning

confidence: 99%

“…Based on this work, for input parameters we take the initial mass of the WDs M WD,i = 1.0, 1.2 M , the initial mass of the He stars M He,i = 1.0-2.8 M , and the initial orbital period log(P orb,i /d) = −1.4 − 0 (see Fig. 3 in Wang et al 2009b). …”

Section: Formation Of Wd + He Star Systemsmentioning

confidence: 99%

“…Recently, Wang et al (2009a) systematically explored the evolution of 2600 close WD binaries that include a He MS star or He subgiant, and obtained the parameter spaces for the progenitor of SNe Ia. With a detailed binary population synthesis approach, Wang et al (2009b) suggested that this channel can contribute a SN Ia birthrate of 3 × 10 −4 yr −1 in the Galaxy, and can result in the short delay times ( < ∼ 100 Myr) between the formation of the progenitor systems and the explosions.…”

Section: Introductionmentioning

confidence: 99%

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

Liu

Chen

Wang

et al. 2010

A&A

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The recent discovery of several overluminous type Ia supernovae (SNe Ia) indicates that the explosive masses of white dwarfs may significantly exceed the canonical Chandrasekhar-mass limit. Rapid differential rotation may support these massive white dwarfs (WDs). Based on the single-degenerate scenario and assuming that the WDs would differentially rotate when the accretion ratė M > 3 × 10 −7 M yr −1 , we performed the numerical calculations for ∼1000 binary systems consisting of a He star and a CO WD with Eggleton's stellar evolution code. We present the initial parameters in the orbital period − helium star-mass plane (for WD masses of 1.0 M and 1.2 M , respectively), which lead to super-Chandrasekhar mass SNe Ia. Our results indicate that for an initially massive WD of 1.2 M , a large number of SNe Ia may result from super-Chandrasekhar mass WDs. The highest mass of the WD at the moment of the SNe Ia explosion is 1.81 M , but very massive (>1.85 M ) WDs cannot be formed. However, when the initial mass of WDs is 1.0 M , the explosive masses of SNe Ia are nearly uniform, which is consistent with the rareness of super-Chandrasekhar mass SNe Ia in observations.

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Type Iax Supernovae

Jha

2017

Handbook of Supernovae

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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 carbonoxygen (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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EVOLVING TO TYPE Ia SUPERNOVAE WITH SHORT DELAY TIMES

Cited by 96 publications

References 80 publications

A progenitor binary and an ejected mass donor remnant of faint type Ia supernovae

A progenitor binary and an ejected mass donor remnant of faint type Ia supernovae

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

Type Iax Supernovae

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