Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau
Close 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 comp...
| Main Authors: | , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/ad354d |
| _version_ | 1797194461234593792 |
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| author | Benjamin M. Tofflemire Lisa Prato Adam L. Kraus Dominique Segura-Cox G. H. Schaefer Rachel Akeson Sean Andrews Eric L. N. Jensen Christopher M. Johns-Krull J. J. Zanazzi M. Simon |
| author_facet | Benjamin M. Tofflemire Lisa Prato Adam L. Kraus Dominique Segura-Cox G. H. Schaefer Rachel Akeson Sean Andrews Eric L. N. Jensen Christopher M. Johns-Krull J. J. Zanazzi M. Simon |
| author_sort | Benjamin M. Tofflemire |
| collection | DOAJ |
| description | Close 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 ${0.35}_{-0.05}^{+0.06}\ {M}_{\odot }$ and 0.34 ± 0.05 M _⊙ for the stellar components, a semimajor axis of $22{\,(}_{-1}^{+2})$ au, and an eccentricity of $0.21{\,(}_{-0.03}^{+0.04})$ . With long-baseline Atacama Large Millimeter/submillimeter Array interferometry, we detect 1.3 mm continuum and ^12 CO ( 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. |
| first_indexed | 2024-04-24T05:56:39Z |
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| id | doaj.art-6387efd428ae4865baaa9e9019ed30c5 |
| institution | Directory Open Access Journal |
| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-04-24T05:56:39Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-6387efd428ae4865baaa9e9019ed30c52024-04-23T08:58:28ZengIOP PublishingThe Astronomical Journal1538-38812024-01-01167523210.3847/1538-3881/ad354dSites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO TauBenjamin M. Tofflemire0https://orcid.org/0000-0003-2053-0749Lisa Prato1https://orcid.org/0000-0001-7998-226XAdam L. Kraus2https://orcid.org/0000-0001-9811-568XDominique Segura-Cox3https://orcid.org/0000-0003-3172-6763G. H. Schaefer4https://orcid.org/0000-0001-5415-9189Rachel Akeson5https://orcid.org/0000-0001-9674-1564Sean Andrews6https://orcid.org/0000-0003-2253-2270Eric L. N. Jensen7https://orcid.org/0000-0002-4625-7333Christopher M. Johns-Krull8https://orcid.org/0000-0002-8828-6386J. J. Zanazzi9https://orcid.org/0000-0002-9849-5886M. Simon10https://orcid.org/0000-0002-4724-2918Department of Astronomy, The University of Texas at Austin , Austin, TX 78712, USA ; tofflemire@utexas.eduLowell Observatory , 1400 West Mars Hill Road, Flagstaff, AZ 86001, USADepartment of Astronomy, The University of Texas at Austin , Austin, TX 78712, USA ; tofflemire@utexas.eduDepartment of Astronomy, The University of Texas at Austin , Austin, TX 78712, USA ; tofflemire@utexas.eduThe CHARA Array of Georgia State University , Mount Wilson Observatory, Mount Wilson, CA 91023, USANASA Exoplanet Science Institute , IPAC/Caltech, Pasadena, CA 91125, USACenter for Astrophysics ∣ Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USADept. of Physics & Astronomy, Swarthmore College , 500 College Avenue, Swarthmore, PA 19081, USAPhysics & Astronomy Department, Rice University , 6100 Main Street, Houston, TX 77005, USAAstronomy Department, Theoretical Astrophysics Center , and Center for Integrative Planetary Science, University of California, Berkeley, CA 94720, USADepartment of Physics and Astronomy, Stony Brook University , Stony Brook, NY 11794, USAClose 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 ${0.35}_{-0.05}^{+0.06}\ {M}_{\odot }$ and 0.34 ± 0.05 M _⊙ for the stellar components, a semimajor axis of $22{\,(}_{-1}^{+2})$ au, and an eccentricity of $0.21{\,(}_{-0.03}^{+0.04})$ . With long-baseline Atacama Large Millimeter/submillimeter Array interferometry, we detect 1.3 mm continuum and ^12 CO ( 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.https://doi.org/10.3847/1538-3881/ad354dYoung stellar objectsProtoplanetary disksBinary starsClose binary stars |
| spellingShingle | Benjamin M. Tofflemire Lisa Prato Adam L. Kraus Dominique Segura-Cox G. H. Schaefer Rachel Akeson Sean Andrews Eric L. N. Jensen Christopher M. Johns-Krull J. J. Zanazzi M. Simon Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau The Astronomical Journal Young stellar objects Protoplanetary disks Binary stars Close binary stars |
| title | Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau |
| title_full | Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau |
| title_fullStr | Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau |
| title_full_unstemmed | Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau |
| title_short | Sites of Planet Formation in Binary Systems. I. Evidence for Disk−Orbit Alignment in the Close Binary FO Tau |
| title_sort | sites of planet formation in binary systems i evidence for disk orbit alignment in the close binary fo tau |
| topic | Young stellar objects Protoplanetary disks Binary stars Close binary stars |
| url | https://doi.org/10.3847/1538-3881/ad354d |
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