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 http://resolver.caltech.edu/CaltechAUTHORS:PATapj08a
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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.
|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.|
|Subject Keywords:||planetary systems : formation; stars : pre-main-sequence|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||07 Jul 2009 22:41|
|Last Modified:||26 Dec 2012 10:53|
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