The helium star donor channel for the progenitors of Type Ia supernovae

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

doi:10.1111/j.1365-2966.2009.14545.x

Cited by 197 publications

(248 citation statements)

References 61 publications

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“…Yoon & Langer (2003) also found that CO WD + He star systems can form a reliable channel that produces SNe Ia. 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: 93%

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

Liu

Chen

Wang

et al. 2010

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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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Section: Introductionmentioning

confidence: 93%

“…Finally, if |Ṁ He | is lower thanṀ low , the strong He-shell flashes occur, and no material can be accumulated onto the WD. Summarizing the above prescriptions, the accumulation efficiency of the accreting He can be written as (Wang et al 2009a)…”

Section: Binary Evolution Codementioning

confidence: 99%

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

Liu

Chen

Wang

et al. 2010

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“…The predicted amount of accreted material is sufficient for the WD to reach the Chandrasekhar limit. This makes HD 49798 another candidate SN Ia progenitor, should the companion be a C/O white dwarf (Wang et al 2009). SN Ia play a key role in the study of cosmic evolution since they are utilised as standard candles for determining the cosmological parameters (e.g.…”

Section: Introductionmentioning

confidence: 99%

The MUCHFUSS project – searching for hot subdwarf binaries with massive unseen companions

Geier

Hirsch

Tillich

et al. 2011

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The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M > 1.0 M ), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.

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“…In the calculations, we adopted the stellar OPAL opacities for a low temperature given by Rogers & Iglesias (1992) and Alexander & Ferguson (1994) and take the ratio of the mixing length to the pressure scale height to be 2.0. The overshooting parameter of the He star (with a chemical abundance Y = 0.98, Z = 0.02) is set to 0 (Wang et al 2009). …”

Section: An Example Evolutionary Path To Psr J1802-2124mentioning

confidence: 99%

He star evolutionary channel to intermediate-mass binary pulsar PSR J1802-2124

Chen

2011

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Context. The intermediate-mass binary pulsars (IMBPs) are characterized by relatively long spin periods (10−200 ms) and massive ( > ∼ 0.4 M ) white dwarf (WD) companions. Recently, precise mass measurements have been performed for the pulsar and the WD in the IMBP PSR J1802-2124. Some observed properties, such as the low mass of the pulsar, the high mass of the WD, the moderately long spin period, and the tight orbit, imply that this system has undergone a peculiar formation mechanism. Aims. In this work, we attempt to simulate the detailed evolutionary history of PSR J1802-2124. Methods. We propose that a binary system consisting of a neutron star (NS, of mass 1.3 M ) and an He star (of mass 1.0 M ), and with an initial orbital period of 0.5 d, may have been the progenitor of PSR J1802-2124. Once the He star overflows its Roche lobe, He-rich material is transferred onto the NS at a relatively high rate of ∼10 −7 −10 −6 M yr −1 , which is significantly higher than the Eddington accretion rate. A large amount of the transferred material is ejected from the vicinity of the NS by radiation pressure and results in the birth of a mildly recycled pulsar. Results. Our simulated results are consistent with the observed parameters of PSR J1802-2124. Therefore, we argue that the NS + He star evolutionary channel may be responsible for the formation of most IMBPs with orbital periods < ∼ 3 d.

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The helium star donor channel for the progenitors of Type Ia supernovae

Cited by 197 publications

References 61 publications

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

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

The MUCHFUSS project – searching for hot subdwarf binaries with massive unseen companions

He star evolutionary channel to intermediate-mass binary pulsar PSR J1802-2124

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