A Caltech Library Service

The evolution of circumstellar disks in Ophiuchus binaries

Patience, J. and Akeson, R. L. and Jensen, E. L. N. (2008) The evolution of circumstellar disks in Ophiuchus binaries. Astrophysical Journal, 677 (1). pp. 616-629. ISSN 0004-637X. doi:10.1086/526394.

PDF - Published Version
See Usage Policy.


Use this Persistent URL to link to this item:


Four Ophiuchus binaries, two Class I systems and two Class II systems, with separations of ~450-1100 AU, were observed with the Owens Valley Radio Observatory (OVRO) millimeter interferometer. In each system, the 3 mm continuum maps show dust emission at the location of the primary star, but no emission at the position of the secondary. This result is different from observations of less evolved Class 0 binaries, in which dust emission is detected from both sources. The nondetection of secondary disks is, however, similar to the dust distribution seen in wide Class II Taurus binaries. The combined OVRO results from the Ophiuchus and Taurus binaries suggest that secondary disk masses are significantly lower than primary disk masses by the Class II stage, with initial evidence that massive secondary disks are reduced by the Class I stage. Although some of the secondaries retain hot inner disk material, the early dissipation of massive outer disks may negatively impact planet formation around secondary stars. Masses for the circumprimary disks are within the range of masses measured for disks around single T Tauri stars and, in some cases, larger than the minimum mass solar nebula. More massive primary disks are predicted by several formation models and are broadly consistent with the observations. Combining the 3 mm data with previous 1.3 mm observations, the dust opacity power-law index for each primary disk is estimated. The opacity index values are all less than the scaling for interstellar dust, possibly indicating grain growth within the circumprimary disks.

Item Type:Article
Related URLs:
URLURL TypeDescription
Akeson, R. L.0000-0001-9674-1564
Jensen, E. L. N.0000-0002-4625-7333
Additional Information:© 2008 The American Astronomical Society. Received 2004 October 12; accepted 2007 November 5. The Owens Valley Millimeter Array is operated by the California Institute of Technology under funding from the National Science Foundation. E. J. gratefully acknowledges support from NSF grant AST-0307830. Funding for J. P. was provided by a Michelson Fellowship from the Michelson Science Center and the NASA Navigator Program. This work made use of the SIMBAD database operated by CDS, France, the NASA Astrophysics Data System, and data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/ California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. We thank members of the OVRO group for valuable discussions on data analysis: H. Arce, J. Carpenter, J. Koda, C. Sanchez-Contreras, and K. Sheth; and we thank H.Arce, M. Bate, L. Looney, R. White, and A. Sargent for productive discussions of the scientific results.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Subject Keywords:planetary systems : formation; stars : pre-main-sequence
Issue or Number:1
Record Number:CaltechAUTHORS:PATapj08a
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13686
Deposited By: Tony Diaz
Deposited On:07 Jul 2009 22:41
Last Modified:08 Nov 2021 22:39

Repository Staff Only: item control page