Asymmetric supernova in hierarchical multiple star systems and application to J1903+0327

Pijloo, Janatie Tjibaria; Caputo, Daniel P.; Zwart, Simon F. Portegies

doi:10.1111/j.1365-2966.2012.21431.x

Cited by 56 publications

(61 citation statements)

References 22 publications

(42 reference statements)

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“…Flannery & van den Heuvel (1975); Sutantyo (1978); Hills (1983); Brandt & Podsiadlowski (1995); Tauris & Bailes (1996); Kalogera (1996); Tauris & Takens (1998); Wex et al (2000); Pijloo et al (2012).…”

Section: General Dynamical Effects Of Snementioning

confidence: 99%

Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

621

690

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Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square-Kilometre-Array searching for radio pulsars and high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most ∼ 0.02 M ⊙ . We investigate DNS masses, spins and velocities, and in particular correlations between spin period, orbital period and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes which may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.

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Section: General Dynamical Effects Of Snementioning

confidence: 99%

Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

621

690

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“…The only previously known eccentric MSP in the Galactic field, PSR J1903+0327 (Champion et al 2008;Freire et al 2011) has a substantially higher eccentricity (  e 0.44) and a 1 M e main-sequence companion. As the latter could not have been responsible for recycling the pulsar, the binary is most likely the remnant of a triple, where the least massive star, responsible for recycling the MSP, was ejected as a result of unstable orbital evolution (Bejger et al 2011;Freire et al 2011;Portegies Zwart et al 2011;Perets & Kratter 2012;Pijloo et al 2012).…”

Section: Introductionmentioning

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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“…Similar calculations have been performed in relation to supernovae in binary (Hills 1983;Tauris & Takens 1998) and triple systems (Pijloo et al 2012).…”

Section: Reconstructing the 1983 Eventmentioning

confidence: 62%

Was the nineteenth century giant eruption of Eta Carinae a merger event in a triple system?

Zwart

Heuvel

2016

Mon. Not. R. Astron. Soc.

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We discuss the events that led to the giant eruption of Eta Carinae, and find that the mid-nineteenth century (in 1838-1843) giant mass-loss outburst has the characteristics of being produced by the merger event of a massive close binary, triggered by the gravitational interaction with a massive third companion star, which is the current binary companion in the Eta Carinae system. We come to this conclusion by a combination of theoretical arguments supported by computer simulations using the Astrophysical Multipurpose Software Environment. According to this model the ∼ 90 M present primary star of the highly eccentric Eta Carinae binary system is the product of this merger, and its ∼ 30 M companion originally was the third star in the system.In our model the Homunculus nebula was produced by an extremely enhanced stellar wind, energized by tidal energy dissipation prior to the merger, which enormously boosted the radiation-driven wind mass-loss. The current orbital plane is then aligned with the equatorial plane of the Homunculus, and the symmetric lobes are roughly aligned with the argument of periastron of the current Eta Carina binary. The merger itself then occurred in 1838, which resulted in a massive asymmetric outflow in the equatorial plane of the Homunculus. The 1843 outburst can in our model be attributed to the subsequent encounter when the companion star (once the outer most star in the triple system) plunges through the bloated envelope of the merger product, once when it passed periastron again. We predict that the system has an excess space velocity of order 50 km/s in the equatorial plane of the Homunculus. Our triple model gives a viable explanation for the high runaway velocities typically observed in LBVs (Smith & Tombleson 2015).

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Asymmetric supernova in hierarchical multiple star systems and application to J1903+0327

Cited by 56 publications

References 22 publications

Formation of Double Neutron Star Systems

Formation of Double Neutron Star Systems

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

Was the nineteenth century giant eruption of Eta Carinae a merger event in a triple system?

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