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Understanding Fomalhaut as a Cooper pair

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Understanding Fomalhaut as a Cooper pair. / Feng, Fabo; Jones, Hugh R. A.

In: Monthly Notices of the Royal Astronomical Society, Vol. 474, No. 4, 11.03.2018, p. 4412-4420.

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@article{5e1975d8b26945b2b68214f45911bf5c,
title = "Understanding Fomalhaut as a Cooper pair",
abstract = "Fomalhaut is a nearby stellar system and has been found to be a triple based on astrometric observations. With new radial velocity and astrometric data, we study the association between Fomalhaut A, B, and C in a Bayesian framework, finding that the system is gravitationally bound or at least associated. Based on simulations of the system, we find that Fomalhaut C can be easily destabilized through combined perturbations from the Galactic tide and stellar encounters. Considering that observing the disruption of a triple is probably rare in the solar neighbourhood, we conclude that Fomalhaut C is a so-called 'gravitational pair' of Fomalhaut A and B. Like the Cooper pair mechanism in superconductors, this phenomenon only appears once the orbital energy of a component becomes comparable with the energy fluctuations caused by the environment. Based on our simulations, we find (1) an upper limit of 8 kms -1 velocity difference is appropriate when selecting binary candidates, and (2) an empirical formula for the escape radius, which is more appropriate than tidal radius when measuring the stability of wide binaries. ",
author = "Fabo Feng and Jones, {Hugh R. A.}",
note = "This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. {\textcopyright} 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.",
year = "2018",
month = mar,
day = "11",
doi = "10.1093/mnras/stx3088",
language = "English",
volume = "474",
pages = "4412--4420",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "4",

}

RIS

TY - JOUR

T1 - Understanding Fomalhaut as a Cooper pair

AU - Feng, Fabo

AU - Jones, Hugh R. A.

N1 - This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

PY - 2018/3/11

Y1 - 2018/3/11

N2 - Fomalhaut is a nearby stellar system and has been found to be a triple based on astrometric observations. With new radial velocity and astrometric data, we study the association between Fomalhaut A, B, and C in a Bayesian framework, finding that the system is gravitationally bound or at least associated. Based on simulations of the system, we find that Fomalhaut C can be easily destabilized through combined perturbations from the Galactic tide and stellar encounters. Considering that observing the disruption of a triple is probably rare in the solar neighbourhood, we conclude that Fomalhaut C is a so-called 'gravitational pair' of Fomalhaut A and B. Like the Cooper pair mechanism in superconductors, this phenomenon only appears once the orbital energy of a component becomes comparable with the energy fluctuations caused by the environment. Based on our simulations, we find (1) an upper limit of 8 kms -1 velocity difference is appropriate when selecting binary candidates, and (2) an empirical formula for the escape radius, which is more appropriate than tidal radius when measuring the stability of wide binaries.

AB - Fomalhaut is a nearby stellar system and has been found to be a triple based on astrometric observations. With new radial velocity and astrometric data, we study the association between Fomalhaut A, B, and C in a Bayesian framework, finding that the system is gravitationally bound or at least associated. Based on simulations of the system, we find that Fomalhaut C can be easily destabilized through combined perturbations from the Galactic tide and stellar encounters. Considering that observing the disruption of a triple is probably rare in the solar neighbourhood, we conclude that Fomalhaut C is a so-called 'gravitational pair' of Fomalhaut A and B. Like the Cooper pair mechanism in superconductors, this phenomenon only appears once the orbital energy of a component becomes comparable with the energy fluctuations caused by the environment. Based on our simulations, we find (1) an upper limit of 8 kms -1 velocity difference is appropriate when selecting binary candidates, and (2) an empirical formula for the escape radius, which is more appropriate than tidal radius when measuring the stability of wide binaries.

UR - http://www.scopus.com/inward/record.url?scp=85040252412&partnerID=8YFLogxK

U2 - 10.1093/mnras/stx3088

DO - 10.1093/mnras/stx3088

M3 - Article

VL - 474

SP - 4412

EP - 4420

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -