The Triple Evolution Dynamical Instability: Stellar Collisions in the Field and the Formation of Exotic Binaries

Perets, Hagai B.; Kratter, Kaitlin M.

doi:10.1088/0004-637x/760/2/99

Cited by 124 publications

(114 citation statements)

References 67 publications

(78 reference statements)

Supporting

Mentioning

109

Contrasting

Order By: Relevance

“…These very eccentric systems may initially have been triple systems in which dynamical instabilities led to the collision between two stars or the ejection of one component and to the formation of eccentric binaries (Perets & Kratter 2012). …”

Section: Our Eccentricity-pumping Modelmentioning

confidence: 99%

Eccentricity-pumping in post-AGB stars with circumbinary discs

Dermine

Izzard

Jorissen

et al. 2013

A&A

112

View full text Add to dashboard Cite

Circumbinary discs are commonly observed around post-asymptotic giant branch (post-AGB) systems and are known to play an important role in their evolution. Several studies have pointed out that a circumbinary disc interacts through resonances with the central binary and leads to angular momentum transfer from the central binary orbit to the disc. This interaction may be responsible for a substantial increase in the binary eccentricity. We investigate whether this disc eccentricity-pumping mechanism can be responsible for the high eccentricities commonly found in post-AGB binary systems.

show abstract

Section: Our Eccentricity-pumping Modelmentioning

confidence: 99%

Eccentricity-pumping in post-AGB stars with circumbinary discs

Dermine

Izzard

Jorissen

et al. 2013

A&A

112

View full text Add to dashboard Cite

show abstract

“…The coalescence of binary companions can occur via orbital disruptions by third bodies (Kozai 1962;Perets & Kratter 2012) or through tidal interactions and Roche Lobe overflow (e.g. Hut 1981).…”

Section: Merger Modelsmentioning

confidence: 99%

The strange evolution of the Large Magellanic Cloud Cepheid OGLE-LMC-CEP1812

Neilson

Izzard

Langer

et al. 2015

A&A

View full text Add to dashboard Cite

Classical Cepheids are key probes of both stellar astrophysics and cosmology as standard candles and pulsating variable stars. It is important to understand Cepheids in unprecedented detail in preparation for upcoming Gaia, James Webb Space Telescope (JWST) and extremely-large telescope observations. Cepheid eclipsing binary stars are ideal tools for achieving this goal, however there are currently only three known systems. One of those systems, OGLE-LMC-CEP1812, raises new questions about the evolution of classical Cepheids because of an apparent age discrepancy between the Cepheid and its red giant companion. We show that the Cepheid component is actually the product of a stellar merger of two main sequence stars that has since evolved across the Hertzsprung gap of the HR diagram. This post-merger product appears younger than the companion, hence the apparent age discrepancy is resolved. We discuss this idea and consequences for understanding Cepheid evolution.

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

The Triple Evolution Dynamical Instability: Stellar Collisions in the Field and the Formation of Exotic Binaries

Cited by 124 publications

References 67 publications

Eccentricity-pumping in post-AGB stars with circumbinary discs

Eccentricity-pumping in post-AGB stars with circumbinary discs

The strange evolution of the Large Magellanic Cloud Cepheid OGLE-LMC-CEP1812

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

Contact Info

Product

Resources

About