The progenitors of type-Ia supernovae in semidetached binaries with red giant donors

Liu, D.; Wang, Bo; Ge, Hongwei; Chen, X.; Han, Zhanwen

doi:10.1051/0004-6361/201833010

Cited by 23 publications

(13 citation statements)

References 99 publications

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“…Li & van den Heuvel 1997;Han & Podsiadlowski 2004;Tauris et al 2013), the present work enlarges the initial parameter regions of WD+RG systems forming WDs with M Ch , especially the initial parameter region in this work containing more massive RG donors. The main reason is that the present work adopted an adiabatic power-law assumptions for the mass-transfer process, which is more reasonable for semidetached binaries with RG donors (see also Liu et al 2019).…”

Section: Comparison To Previous Studiesmentioning

confidence: 99%

Formation of millisecond pulsars with long orbital periods by accretion-induced collapse of white-dwarfs

Wang,

Liu,

Chen

2022

Preprint

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Accretion-induced collapse (AIC) of massive white-dwarfs (WDs) has been proposed as an important way for the formation of neutron star (NS) systems. An oxygen-neon (ONe) WD that accretes H-rich material from a red-giant (RG) star may experience the AIC process, eventually producing millisecond pulsars (MSPs), known as the RG donor channel. Previous studies indicate that this channel can only account for MSPs with orbital periods > 500 d. It is worth noting that some more MSPs with wide orbits (60−500 d) have been detected by recent observations, but their origin is still highly uncertain. In the present work, by employing an adiabatic power-law assumptions for the mass-transfer process, we performed a large number of complete binary evolution calculations for the formation of MSPs through the RG donor channel in a systematic way. We found that this channel can contribute to the observed MSPs with orbital periods in the range of 50 − 1200 d, and almost all the observed MSPs with wide orbits can be covered by this channel in the WD companion mass versus orbital period diagram. The present work indicates that the AIC process provides a viable way to form MSPs with wide orbits.

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Section: Comparison To Previous Studiesmentioning

confidence: 99%

Formation of millisecond pulsars with long orbital periods by accretion-induced collapse of white-dwarfs

Wang,

Liu,

Chen

2022

Preprint

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“…By adopting a power-law adiabatic supposition for the mass-transfer prescription that can be well applicable for the mass-transfer process from a RG donor (e.g., Ge et al 2010 recently enlarged the parameter space of WD+RG systems for producing WDs with M Ch . It seems that the adiabatic mass-transfer prescription for RG donor is still highly uncertain (e.g., Woods & Ivanova 2011), but the work by Liu et al (2019) at least provides an upper limit for the parameter regions that can form WDs with M Ch . Fig.…”

Section: Parameter Space For Aic Eventsmentioning

confidence: 99%

The formation of neutron star systems through accretion-induced collapse in white-dwarf binaries

Wang,

Liu

2020

Preprint

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The accretion-induced collapse (AIC) scenario was proposed 40 years ago as an evolutionary end state of oxygen-neon white-dwarfs (ONe WDs), linking them to the formation of neutron star (NS) systems. However, there has been no direct detection of any AIC event so far, even though there exists a lot of indirect observational evidence. Meanwhile, the binary evolutionary pathways resulting in NS formation through AIC are still not well investigated. In this article, we review recent studies on the two classic progenitor models of AIC events, i.e., the single-degenerate model (including the ONe WD+MS/RG/He star channels and the CO WD+He star channel) and the doubledegenerate model (including the double CO WD channel, the double ONe WD channel and the ONe WD+CO WD channel). Recent progress on these progenitor models is reviewed, including the binary evolutionary scenarios leading to AIC events, the initial parameter space for producing AIC events, and the related objects (e.g., the pre-AIC systems and the post-AIC systems). For the single-degenerate model, the pre-AIC systems (i.e., the progenitor systems of AIC events) could potentially be identified as cataclysmic variables (such as classical novae, recurrent novae, Ne novae and He novae), symbiotics and supersoft X-ray sources in the observations, whereas the post-AIC systems (i.e., NS systems) could potentially be identified as low-/intermediate-mass X-ray binaries, and the resulting low-/intermediate-mass binary pulsars, most notably millisecond pulsars. For the double-degenerate model, the pre-AIC systems are close double WDs with short orbital periods, whereas the post-AIC systems are single isolated NSs that may correspond to a specific kind of NS with peculiar properties. We also review the predicted rates of AIC events, the mass distribution of NSs produced via AIC, and the gravitational wave (GW) signals from double WDs that are potential GW sources in the Galaxy in the context of future space-based GW detectors, such as LISA, TianQin and Taiji, etc. Recent theoretical and observational constraints on the detection of AIC events are summarized. In order to confirm the existence of the AIC process, and resolve this long-term issue presented by current stellar evolution theories, more numerical simulations and observational identifications are required.

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“…Claeys et al (2014) and Wang et al (2015) simulated the CO WD and main sequence star (CO WD+MS) channel, and found most of the SNe Ia are produced in 10 8 ∼ 10 9 years after star formation. Liu et al (2019) simulated the CO WD and red giant star (CO WD+RG) channel, and found the delay time to be 10 8.6 ∼ 10 8.7 years but with a steeper delay time relation than that of the DD scenario. Apart from MS or RG serving as the companion star, Wang et al (2017) simulated CO WD + He star as SN Ia progenitor system, which shows a peak of the event rate around 10 8 years.…”

Section: Introductionmentioning

confidence: 99%

Constraining Type Ia Supernova Delay Time with Spatially Resolved Star Formation Histories

Chen,

Hu,

Wang

2021

Preprint

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We present the delay time distribution (DTD) estimates of Type Ia supernovae (SNe Ia) using spatially resolved SN Ia host galaxy spectra from MUSE and MaNGA. By employing a grouping algorithm based on k-means and earth mover's distances (EMD), we separated the host galaxy star formation histories (SFHs) into spatially distinct regions and used maximum likelihood method to constrain the DTD of SNe Ia progenitors. When a power-law model of the form DT D(t) ∝ t s (t > τ ) is used, we found an SN rate decay slope s = −1.41 +0.32 −0.33 and a delay time τ = 120 +142 −83 M yr . Moreover, we tested other DTD models such as a broken power law model and a two-component power law model, and found no statistically significant support to these alternative models.

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The progenitors of type-Ia supernovae in semidetached binaries with red giant donors

Cited by 23 publications

References 99 publications

Formation of millisecond pulsars with long orbital periods by accretion-induced collapse of white-dwarfs

Formation of millisecond pulsars with long orbital periods by accretion-induced collapse of white-dwarfs

The formation of neutron star systems through accretion-induced collapse in white-dwarf binaries

Constraining Type Ia Supernova Delay Time with Spatially Resolved Star Formation Histories

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