Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau

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dc.citation.articleNumber232en_US
dc.citation.issueNumber5en_US
dc.citation.journalTitleThe Astronomical Journalen_US
dc.citation.volumeNumber167en_US
dc.contributor.authorTofflemire, Benjamin M.en_US
dc.contributor.authorPrato, Lisaen_US
dc.contributor.authorKraus, Adam L.en_US
dc.contributor.authorSegura-Cox, Dominiqueen_US
dc.contributor.authorSchaefer, G. H.en_US
dc.contributor.authorAkeson, Rachelen_US
dc.contributor.authorAndrews, Seanen_US
dc.contributor.authorJensen, Eric L. N.en_US
dc.contributor.authorJohns-Krull, Christopher M.en_US
dc.contributor.authorZanazzi, J. J.en_US
dc.contributor.authorSimon, M.en_US
dc.date.accessioned2024-07-25T20:55:16Zen_US
dc.date.available2024-07-25T20:55:16Zen_US
dc.date.issued2024en_US
dc.description.abstractClose binary systems present challenges to planet formation. As binary separations decrease, so do the occurrence rates of protoplanetary disks in young systems and planets in mature systems. For systems that do retain disks, their disk masses and sizes are altered by the presence of the binary companion. Through the study of protoplanetary disks in binary systems with known orbital parameters, we seek to determine the properties that promote disk retention and therefore planet formation. In this work, we characterize the young binary−disk system FO Tau. We determine the first full orbital solution for the system, finding masses of and 0.34 ± 0.05 M ⊙ for the stellar components, a semimajor axis of au, and an eccentricity of . With long-baseline Atacama Large Millimeter/submillimeter Array interferometry, we detect 1.3 mm continuum and 12CO (J = 2–1) line emission toward each of the binary components; no circumbinary emission is detected. The protoplanetary disks are compact, consistent with being truncated by the binary orbit. The dust disks are unresolved in the image plane, and the more extended gas disks are only marginally resolved. Fitting the continuum and CO visibilities, we determine the inclination of each disk, finding evidence for alignment of the disk and binary orbital planes. This study is the first of its kind linking the properties of circumstellar protoplanetary disks to a precisely known binary orbit. In the case of FO Tau, we find a dynamically placid environment (coplanar, low eccentricity), which may foster its potential for planet formation.en_US
dc.identifier.citationTofflemire, B. M., Prato, L., Kraus, A. L., Segura-Cox, D., Schaefer, G. H., Akeson, R., Andrews, S., Jensen, E. L. N., Johns-Krull, C. M., Zanazzi, J. J., & Simon, M. (2024). Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau. The Astronomical Journal, 167(5), 232. https://doi.org/10.3847/1538-3881/ad354den_US
dc.identifier.digitalTofflemire_2024_AJ_167_232en_US
dc.identifier.doihttps://doi.org/10.3847/1538-3881/ad354den_US
dc.identifier.urihttps://hdl.handle.net/1911/117505en_US
dc.language.isoengen_US
dc.publisherIOP Publishingen_US
dc.rightsExcept where otherwise noted, this work is licensed under a Creative Commons Attribution (CC BY) license.  Permission to reuse, publish, or reproduce the work beyond the terms of the license or beyond the bounds of fair use or other exemptions to copyright law must be obtained from the copyright holder.en_US
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/en_US
dc.titleSites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tauen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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