Accretion-induced Collapse from Helium Star + White Dwarf Binaries

Brooks, Jared; Schwab, Josiah; Bildsten, Lars; Quataert, Eliot; Paxton, Bill

doi:10.3847/1538-4357/aa79a6

Cited by 46 publications

(52 citation statements)

References 41 publications

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“…But this presumably converts the entire C/O core into O/Ne (Nomoto & Iben 1985;Lecoanet et al 2016). For an initially O/Ne core, this flame converts the C/O shell to O/Ne (Brooks et al 2017).…”

Section: Mesa Modelsmentioning

confidence: 99%

Fast and Luminous Transients from the Explosions of Long-lived Massive White Dwarf Merger Remnants

Brooks

Schwab

Bildsten

et al. 2017

ApJ

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We study the evolution and final outcome of long-lived (≈10 5 years) remnants from the merger of a He white dwarf (WD) with a more massive C/O or O/Ne WD. Using Modules for Experiments in Stellar Astrophysics (MESA), we show that these remnants have a red giant configuration supported by steady helium burning, adding mass to the WD core until it reaches M core ≈ 1.12 − 1.20M . At that point, the base of the surface convection zone extends into the burning layer, mixing the helium burning products (primarily carbon and magnesium) throughout the convective envelope. Further evolution depletes the convective envelope of helium, and dramatically slows the mass increase of the underlying WD core. The WD core mass growth re-initiates after helium depletion, as then an uncoupled carbon burning shell is ignited and proceeds to burn the fuel from the remaining metal-rich extended envelope. For large enough initial total merger masses, O/Ne WD cores would experience electron-capture triggered collapse to neutron stars (NSs) after growing to near Chandrasekhar mass (M Ch ). Massive C/O WD cores could suffer the same fate after a carbon-burning flame converts them to O/Ne. The NS formation would release ≈10 50 ergs into the remaining extended low mass envelope. Using the STELLA radiative transfer code, we predict the resulting optical light curves from these exploded envelopes. Reaching absolute magnitudes of M V ≈ −17, these transients are bright for about one week, and have many features of the class of luminous, rapidly evolving transients studied by Drout and collaborators.

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Section: Mesa Modelsmentioning

confidence: 99%

Fast and Luminous Transients from the Explosions of Long-lived Massive White Dwarf Merger Remnants

Brooks

Schwab

Bildsten

et al. 2017

ApJ

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“…Brooks et al (2016) calculated full binary evolution of WD+He star systems, whereas we suppose that off-centre carbon burning occurs if the mass-transfer rate is higher thanṀcr. Note that the results obtained here are very similar to those of Brooks et al (2016).…”

Section: Discussionmentioning

confidence: 99%

“…The minimum delay time in Figure 4 is determined by the MS lifetime of a 8 M ⊙ star, which is the maximum mass of a star able to form CO WDs. Brooks et al (2016) recently also reported these two possible outcomes (i.e., centre or off-centre carbon ignition), but they calculated over a narrower range of parameter space.…”

Section: Birthrates Of Sne Iamentioning

confidence: 99%

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The WD+He star binaries as the progenitors of type Ia supernovae

Wang

Liu

2017

Open Astronomy

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Employing the MESA stellar evolution code, we computed He accretion onto carbon-oxygen white dwarfs (CO WDs). We found two possible outcomes for models in which the WD steadily grows in mass towards the Chandrasekhar limit. For relatively low He-accretion rates carbon ignition occurs in the center, leading to a type Ia supernova (SN Ia) explosion, whereas for relatively high accretion rates carbon is ignited off-center, probably leading to collapse. Thus the parameter space producing SNe Ia is reduced compared to what was assumed in earlier papers, in which the possibility of off-center ignition was ignored. We then applied these results in binary population synthesis modelling, finding a modest reduction in the expected birthrate of SNe Ia resulting from the WD+He star channel.

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“…This mild expansion is not enough to power mass loss, but is enough to temporarily prevent surface accretion. This can be seen in Figure 4, which shows the mass transfer rate by the dotted black line and the WD mass accretion rate by the solid black line, which has sharp dips caused by the carbon burning flashes (Brooks et al 2017).…”

Section: Wd Companionmentioning

confidence: 90%

HD 49798: Its History of Binary Interaction and Future Evolution

Brooks

Kupfer

Bildsten

2017

ApJ

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The bright subdwarf-O star (sdO) HD 49798 is in a 1.55 day orbit with a compact companion that is spinning at 13.2 s. Using the measurements of the effective temperature (T eff ), surface gravity ( g log ), and surface abundances of the sdO, we construct models to study the evolution of this binary system using Modules for Experiments in Stellar Astrophysics (MESA). Previous studies of the compact companion have disagreed on whether it is a white dwarf (WD) or a neutron star (NS). From the published measurements of the companion's spin and spin-up rate, we agree with Mereghetti and collaborators that an NS companion is more likely. However, since there remains the possibility of a WD companion, we use our constructed MESA models to run simulations with both WD and NS companions that help us constrain the past and future evolution of this system. If it presently contains an NS, the immediate mass transfer evolution upon Roche lobe filling will lead to mass transfer rates comparable to that implied in ultraluminous X-ray sources (ULXs). Depending on the rate of angular momentum extraction via a wind, the fate of this system is either a wide ( » P 3 orb day) intermediate-mass binary pulsar (IMPB) with a relatively rapidly spinning NS (≈0.3 s) and a high mass WD (»  M 0.9 ), or a solitary millisecond pulsar (MSP).

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Accretion-induced Collapse from Helium Star + White Dwarf Binaries

Cited by 46 publications

References 41 publications

Fast and Luminous Transients from the Explosions of Long-lived Massive White Dwarf Merger Remnants

Fast and Luminous Transients from the Explosions of Long-lived Massive White Dwarf Merger Remnants

The WD+He star binaries as the progenitors of type Ia supernovae

HD 49798: Its History of Binary Interaction and Future Evolution

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