A Strange Star Scenario for the Formation of Eccentric Millisecond Pulsar/Helium White Dwarf Binaries

Jiang, L.; Li, Xiang-Dong; Dey, Jishnu; Dey, Mira

doi:10.1088/0004-637x/807/1/41

Cited by 34 publications

(39 citation statements)

References 97 publications

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“…In addition, the pulsar mass (Table 2) contradicts the quark-nova formation theory proposed by Jiang et al (2015). Combined with the inferred peculiar velocity, it also poses stringent constraints on the rotationally delayed AIC hypothesis of Freire & Tauris (2014), as the latter requires both a differentially rotating super-Chandrasekhar-mass WD progenitor and asymmetric mass loss at birth.…”

Section: Discussionmentioning

confidence: 90%

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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: Discussionmentioning

confidence: 90%

“…A possible explanation for the observed eccentricities is a spontaneous phase transition of either a super-Chandrasekhar WD collapsing into an NS (Freire & Tauris 2014), or of an NS imploding into a strange-quark star (Jiang et al 2015). In either case, the transformation is mass-critical and therefore the pulsar masses should be similar.…”

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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“…showing clear rapid orbital decay consistent with general relativity prediction due to gravitational wave radiation. White dwarfs have been identified as companions to millisecond pulsars [64][65][66][67][68][69][70][71][72][73][74][75][76] . Ref.…”

Section: Dzsmentioning

confidence: 99%

White Dwarf Stars

Romero

Pelisoli

Ourique

2017

Int. J. Mod. Phys. Conf. Ser.

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White dwarf stars are the final stage of most stars, born single or in multiple systems. We discuss the identification, magnetic fields, and mass distribution for white dwarfs detected from spectra obtained by the Sloan Digital Sky Survey up to Data Release 13 in 2016, which lead to the increase in the number of spectroscopically identified white dwarf stars from 5 000 to 39 000. This number includes only white dwarf stars with log g ≥ 6.5, i.e., excluding the Extremely Low Mass white dwarfs, which are necessarily the byproduct of stellar interaction.

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“…The ideas for such a mechanism explored in the past include the enhanced mass loss and transfer during the periastron passages (Soker 2000;Bonačić-Marinović et al 2008) and kicks received by the WD at birth (Izzard et al 2010). Eccentric binary MSPs were also suggested to originate from the dynamical evolution in a triple stellar system (Portegies Zwart et al 2011), accretion-induced collapse (Freire & Tauris 2014), and quark nova (Jiang et al 2015).…”

Section: Introductionmentioning

confidence: 99%

On the Eccentricity Excitation in Post-Main-Sequence Binaries

Rafikov

2016

ApJ

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Several classes of stellar binaries with post-main-sequence (post-MS) components-millisecond pulsars with the white dwarf companions (MSP+WD) and periods ofP 30 b days, binaries hosting post-asymptotic giant branch stars, or barium stars withP b several years-feature high eccentricities (up to 0.4) despite the expectation of their efficient tidal circularization during their post-MS evolution. It was suggested that the eccentricities of these binaries can be naturally excited by their tidal coupling to the circumbinary disk, formed by the material ejected from the binary. Here we critically reassess this idea using simple arguments rooted in the global angular momentum conservation of the disk+binary system. Compared to previous studies, we (1) fully account for the viscous spreading of the circumbinary disk, (2) consider the possibility of reaccretion from the disk onto the binary (in agreement with simulations and empirical evidence), and (3) allow for the reduced viscosity after the disk expands, cools, and forms dust. These ingredients conspire to significantly lower the efficiency of eccentricity excitation by the disk tides. We find that explaining eccentricities of the post-MS binaries is difficult and requires massive ( - M 10 2 ), long-lived (10 5 years) circumbinary disks that do not reaccrete. While disk tides may account for the eccentricities of the MSP+WD binaries, we show reaccretion to also be detrimental for these systems. Reduced efficiency of the disk-driven excitation motivates thestudy of alternative mechanisms for producing the peculiar eccentricities of the post-MS binaries.

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A Strange Star Scenario for the Formation of Eccentric Millisecond Pulsar/Helium White Dwarf Binaries

Cited by 34 publications

References 97 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

White Dwarf Stars

On the Eccentricity Excitation in Post-Main-Sequence Binaries

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