Simulations of the Fomalhaut system within its local galactic environment

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dc.contributor.authorKaib, Nathan A.
dc.contributor.authorWhite, Ethan B.
dc.contributor.authorIzidoro, André [UNESP]
dc.contributor.institutionUniversity of Oklahoma
dc.contributor.institutionUniversidade Estadual Paulista (Unesp)
dc.date.accessioned2018-12-11T16:53:04Z
dc.date.available2018-12-11T16:53:04Z
dc.date.issued2018-01-01
dc.description.abstractFomalhaut A is among the most well-studied nearby stars and has been discovered to possess a putative planetary object as well as a remarkable eccentric dust belt. This eccentric dust belt has often been interpreted as the dynamical signature of one or more planets that elude direct detection. However, the system also contains two other stellar companions residing ~ 105 au from Fomalhaut A. We have designed a new symplectic integration algorithm to model the evolution of Fomalhaut A's planetary dust belt in concert with the dynamical evolution of its stellar companions to determine if these companions are likely to have generated the dust belt's morphology. Using our numerical simulations, we find that close encounters between Fomalhaut A and B are expected, with an ~ 25 per cent probability that the two stars have passed within at least 400 au of each other at some point. Although the outcomes of such encounter histories are extremely varied, these close encounters nearly always excite the eccentricity of Fomalhaut A's dust belt and occasionally yield morphologies very similar to the observed belt. With these results, we argue that close encounters with Fomalhaut A's stellar companions should be considered a plausible mechanism to explain its eccentric belt, especially in the absence of detected planets capable of sculpting the belt's morphology. More broadly, we can also conclude from this work that very wide binary stars may often generate asymmetries in the stellar debris discs they host.en
dc.description.affiliationHL Dodge Department of Physics and Astronomy University of Oklahoma
dc.description.affiliationUNESP Univ. Estadual Paulista Grupo de Dinâmica Orbital and Planetologia
dc.description.affiliationUnespUNESP Univ. Estadual Paulista Grupo de Dinâmica Orbital and Planetologia
dc.format.extent470-491
dc.identifierhttp://dx.doi.org/10.1093/MNRAS/STX2456
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, v. 473, n. 1, p. 470-491, 2018.
dc.identifier.doi10.1093/MNRAS/STX2456
dc.identifier.file2-s2.0-85046072517.pdf
dc.identifier.issn1365-2966
dc.identifier.issn0035-8711
dc.identifier.scopus2-s2.0-85046072517
dc.identifier.urihttp://hdl.handle.net/11449/170941
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.relation.ispartofsjr2,346
dc.relation.ispartofsjr2,346
dc.rights.accessRightsAcesso aberto
dc.sourceScopus
dc.subjectBinaries: visual
dc.subjectCircumstellar matter
dc.subjectMethods: numerical
dc.subjectPlanet-disc interactions
dc.subjectPlanets and satellites: dynamical evolution and stability
dc.subjectStars: kinematics and dynamics
dc.titleSimulations of the Fomalhaut system within its local galactic environmenten
dc.typeArtigo

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