Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Tauris, T. M.; Sanyal, D.; Yoon, Sung‐Chul; Langer, N.

doi:10.1051/0004-6361/201321662

Cited by 141 publications

(192 citation statements)

References 165 publications

(229 reference statements)

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“…An alternative mechanism proposed by Freire & Tauris (2014) theorizes that eMSPs form indirectly from a rotationally delayed accretion-induced collapse (AIC) of a massive WD. First, because WDs require a fine-tuned mass transfer rate to grow in mass (Nomoto & Kondo 1991;Chen et al 2011;Tauris et al 2013), the resultant systems are expected to have orbital periods in the 10-60 day range, in agreement with the known eMSPs. Freire & Tauris (2014) propose that the AIC could in principle be delayed until after the cessation of mass transfer, due to the rapid rotation of the WD progenitor.…”

Section: Origin and Evolutionmentioning

confidence: 99%

An Eccentric Binary Millisecond Pulsar With a Helium White Dwarf Companion in the Galactic Field

Antoniadis

Kaplan

Stovall

et al. 2016

ApJ

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Low-mass white dwarfs (LMWDs) are believed to be exclusive products of binary evolution, as the universe is not old enough to produce them from single stars. Because of the strong tidal forces operating during the binary interaction phase, the remnant systems observed today are expected to have negligible eccentricities. Here, we report on the first unambiguous identification of an LMWD in an eccentric (e=0.13) orbit around the millisecond pulsar PSR J2234+0511, which directly contradicts this picture. We use our spectra and radio-timing solution (derived elsewhere) to infer the WD temperature ( =  T 8600 190 eff K), and peculiar systemic velocity relative to the local standard of rest (31 km s −1). We also place model-independent constraints on the WD radius . The WD and kinematic properties are consistent with the expectations for low-mass X-ray binary evolution and disfavor a dynamic three-body formation channel. In the case of the high eccentricity being the result of a spontaneous phase transition, we infer a mass of ∼1.60 M e for the pulsar progenitor, which is too low for the quark-nova mechanism proposed by Jiang et al., and too high for the scenario of Freire & Tauris, in which a WD collapses into a neutron star via a rotationally delayed accretion-induced collapse. We find that eccentricity pumping via interaction with a circumbinary disk is consistent with our inferred parameters. Finally, we report tentative evidence for pulsations that, if confirmed, would transform the star into an unprecedented laboratory for WD physics.

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Section: Origin and Evolutionmentioning

confidence: 99%

An Eccentric Binary Millisecond Pulsar With a Helium White Dwarf Companion in the Galactic Field

Antoniadis

Kaplan

Stovall

et al. 2016

ApJ

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“…Many pulsars are observed in globular clusters which have small escape velocities of 40 km s −1 . Theoretical studies of electron capture SNe and the accretion-induced collapse (AIC) of massive WDs provide a plausible NS formation mechanism which predicts a low kick velocity (Podsiadlowski et al 2004;Schwab et al 2010;Tauris et al 2013b). In addition, there is the interesting question of a possible alignment at birth between the pulsar velocity vector and its spin axis, as suggested by recent observational evidence and modelling (Noutsos et al 2013).…”

Section: Neutron Star Kicks and Velocitiesmentioning

confidence: 99%

Understanding the Neutron Star Population with the SKA

Tauris¹,

Kaspi²,

Breton³

et al. 2015

Proceedings of Advancing Astrophysics With the Square Kilometre Array — PoS(AASKA14)

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Since their discovery in the late 1960's the population of known neutron stars has grown to ∼2500. This sample has yielded many surprises and demonstrated that the observational properties of neutron stars are remarkably diverse. The surveys that will be performed with the SKA will produce a further tenfold increase in the number of Galactic neutron stars known. Moreover, the SKA's broad spectral coverage, sub-arraying and multi-beaming capabilities will allow us to characterise these sources with unprecedented efficiency, in turn enabling a giant leap in the understanding of their properties. We review the neutron star population and outline strategies for studying each of the growing number of diverse classes that are populating the "neutron star zoo". Questions that will be addressed by the much larger statistical samples and vastly improved timing efficiency provided by SKA include: (i) the spin period and spin-down rate distributions (and thus magnetic fields) at birth, and the associated information about the supernovae wherein they are formed; (ii) the radio pulsar-magnetar connection; (iii) the link between normal radio pulsars, intermittent pulsars and rotating radio transients; (iv) the slowest possible spin period for a radio pulsar (revealing the conditions at the pulsar death-line); (v) proper motions of pulsars (revealing supernova kick physics); (vi) the mass distribution of neutron stars; (vii) the fastest possible spin period for a recycled pulsar (constraining magnetosphere-accretion disc interactions, gravitational wave radiation and the equation-of-state); (viii) the origin of high eccentricity millisecond pulsars; (ix) the formation channels for recently identified triple systems; and finally (x) how isolated millisecond pulsars are formed. We can also expect that the first phase of the SKA (SKA1), and in particular the full SKA (SKA2), will break new ground unveiling exotic and heretofore unknown systems that will challenge our current knowledge and theories, thus fostering the development of new research areas. Some possibilities for future landmark discoveries representing significant milestones in the astrophysics of compact objects include: (i) sub-millisecond pulsars; (ii) neutron stars born as millisecond pulsars; (iii) neutron stars with masses below 1.1 or above 2.5 M ; (iv) neutron star-black hole binaries; and (v) a triple system containing a pair of neutron stars.Advancing Astrophysics with the Square Kilometre Array

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“…AIC supernovae are predicted to be very fast and faint (Woosley & Baron 1992;Dessart et al 2006) and thus difficult to observe. The remnant NSs may, however, be detectable as low-mass binary pulsars (Nomoto & Kondo 1991), or, if they are later spun up by accretion, millisecond pulsars (MSPs) (Tauris et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Accretion-induced Collapse from Helium Star + White Dwarf Binaries

Brooks

Schwab

Bildsten

et al. 2017

ApJ

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Accretion-induced collapse (AIC) occurs when an O/Ne white dwarf (WD) grows to nearly the Chandrasekhar mass (M Ch ), reaching central densities that trigger electron captures in the core. Using Modules for Experiments in Stellar Astrophysics (MESA), we present the first true binary simulations of He star + O/Ne WD binaries, focusing on a 1.5M He star in a 3 hour orbital period with 1.1−1.3M O/Ne WDs. The helium star fills its Roche lobe after core helium burning is completed and donates helium on its thermal timescale to the WD,Ṁ ≈ 3 × 10 −6 M /yr, a rate high enough that the accreting helium burns stably on the WD. The accumulated carbon/oxygen ashes from the helium burning undergo an unstable shell flash that initiates an inwardly moving carbon burning flame. This flame is only quenched when it runs out of carbon at the surface of the original O/Ne core. Subsequent accumulation of fresh carbon/oxygen layers also undergo thermal instabilities, but no mass loss is triggered, allowing M WD → M Ch , triggering the onset of AIC. We also discuss the scenario of accreting C/O WDs that experience shell carbon ignitions to become O/Ne WDs, and then, under continuing mass transfer, lead to AIC. Studies of the AIC event rate using binary population synthesis should include all of these channels, especially this latter channel, which has been previously neglected but might dominate the rate.

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Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Cited by 141 publications

References 165 publications

An Eccentric Binary Millisecond Pulsar With a Helium White Dwarf Companion in the Galactic Field

An Eccentric Binary Millisecond Pulsar With a Helium White Dwarf Companion in the Galactic Field

Understanding the Neutron Star Population with the SKA

Accretion-induced Collapse from Helium Star + White Dwarf Binaries

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