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Dynamics of passing-stars-perturbed binary star systems
Univ Vienna, Inst Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
Uppsala University, Disciplinary Domain of Science and Technology, Physics, Department of Physics and Astronomy, Theoretical Astrophysics. Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT 2511, Australia.ORCID iD: 0000-0001-5344-8069
Univ Vienna, Inst Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
Univ Vienna, Inst Astrophys, Turkenschanzstr 17, A-1180 Vienna, Austria.
2019 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 486, no 4, p. 4773-4780Article in journal (Refereed) Published
Abstract [en]

In this work, we investigate the dynamical effects of a sequence of close encounters over 200 Myr varying in the interval of 10 000-100 000 au between a binary star system and passing stars with masses ranging from 0.1 to 10 M-circle dot. We focus on binaries consisting of two Sun-like stars with various orbital separations a(0) from 50 to 200 au initially on circular planar orbits. We treat the probletn statistically since each sequence is clotted 1000 dines. Our study shows that orbits of binaries initially at a(0) = 50 au will slightly be perturbed by each close encounter and exhibit a small deviation in eccentricity (+0.03) and in periapsis distance (+1 and -2 au) around the mean value, However increasing a(0) will drastically increase these variances: up to +0.45 in eccentricity and between +63 and -106 au in periapsis, leading to a higher rate of disrupted binaries up to 50 per cent after the sequence of close encounters. Even though the secondary star can remain bound to the primary, similar to 20 per cent of the final orbits will have inclinations greater than 10 degrees. As planetary formation already takes place when stars are still members of their birth cluster, we show that the variances in eccentricity and periapsis distance of Jupiter- and Saturn-like planets will inversely decrease with a(0) after successive fly-bys. This leads to higher ejection rate at a(0) = 50 au but to a higher extent for Saturn-likes (60 percent) as those planets' apoapsis distances cross the critical stability distance for such binary separation.

Place, publisher, year, edition, pages
2019. Vol. 486, no 4, p. 4773-4780
Keywords [en]
methods: numerical, methods: statistical, celestial mechanics, binaries: general
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:uu:diva-390978DOI: 10.1093/mnras/stz1173ISI: 000474908200023OAI: oai:DiVA.org:uu-390978DiVA, id: diva2:1343875
Available from: 2019-08-19 Created: 2019-08-19 Last updated: 2019-08-19Bibliographically approved

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