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The frequency of binary star interlopers amongst transitional discs

Ruiz Rodriguez, Dary; Cieza, Lucas A; Kraus, A L; Ireland, Michael

Description

Using Non-Redundant Mask interferometry (NRM), we searched for binary companions to objects previously classified as transitional discs (TD). These objects are thought to be an evolutionary stage between an optically thick disc and optically thin disc. We investigate the presence of a stellar companion as a possible mechanism of material depletion in the inner region of these discs, which would rule out an ongoing planetary formation process in distances comparable to the binary separation. For...[Show more]

dc.contributor.authorRuiz Rodriguez, Dary
dc.contributor.authorCieza, Lucas A
dc.contributor.authorKraus, A L
dc.contributor.authorIreland, Michael
dc.date.accessioned2018-11-29T22:53:59Z
dc.date.available2018-11-29T22:53:59Z
dc.identifier.issn0035-8711
dc.identifier.urihttp://hdl.handle.net/1885/152637
dc.description.abstractUsing Non-Redundant Mask interferometry (NRM), we searched for binary companions to objects previously classified as transitional discs (TD). These objects are thought to be an evolutionary stage between an optically thick disc and optically thin disc. We investigate the presence of a stellar companion as a possible mechanism of material depletion in the inner region of these discs, which would rule out an ongoing planetary formation process in distances comparable to the binary separation. For our detection limits, we implement a new method of completeness correction using a combination of randomly sampled binary orbits and Bayesian inference. The selected sample of 24 TDs belongs to the nearby and young star-forming regions: Ophiuchus (˜130 pc), Taurus-Auriga (˜140 pc) and IC348 (˜220 pc). These regions are suitable to resolve faint stellar companions with moderate to high confidence levels at distances as low as 2 au from the central star. With a total of 31 objects, including 11 known TDs and circumbinary discs from the literature, we have found that a fraction of 0.38 ± 0.09 of the SEDs of these objects are likely due to the tidal interaction between a close binary and its disc, while the remaining SEDs are likely the result of other internal processes such as photoevaporation, grain growth, planet-disc interactions. In addition, we detected four companions orbiting outside the area of the truncation radii and propose that the IR excesses of these systems are due to a disc orbiting a secondary companion.
dc.format.mimetypeapplication/pdf
dc.publisherBlackwell Publishing Ltd
dc.sourceMonthly Notices of the Royal Astronomical Society
dc.titleThe frequency of binary star interlopers amongst transitional discs
dc.typeJournal article
local.description.notesImported from ARIES
local.identifier.citationvolume463
dc.date.issued2016
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationu5227626xPUB6
local.type.statusPublished Version
local.contributor.affiliationRuiz Rodriguez, Dary, College of Science, ANU
local.contributor.affiliationIreland, Michael, College of Science, ANU
local.contributor.affiliationCieza, Lucas A, University of Hawaii
local.contributor.affiliationKraus, A L, The University of Texas
local.bibliographicCitation.issue4
local.bibliographicCitation.startpage3829
local.bibliographicCitation.lastpage3847
local.identifier.doi10.1093/mnras/stw2297
dc.date.updated2018-11-29T07:56:47Z
local.identifier.thomsonID000393568200031
dcterms.accessRightsOpen Access
CollectionsANU Research Publications

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