Dusty disks in the multiple systems UZ Tauri and GG Tauri

Details Dusty disks in the multiple systems UZ Tauri and GG Tauri Dusty disks in the multiple systems UZ Tauri and GG Tauri

Sep 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...397l..47s&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 397, no. 1, p. L47-L49.

Astronomy and Astrophysics

Astrophysics

31

Binary Stars, Cosmic Dust, Stellar Systems, T Tauri Stars, Thermal Emission, Triple Stars, Astronomical Models, Emission Spectra, Optical Thickness, Star Formation

Scientific paper

Interferometric observations of the 2.6 mm dust thermal emission around the T Tauri triple system UZ Tau show that most of it is equally divided between UZ Tau W (the close binary) and UZ Tau E. The emission is at least partially optically thick at 2.6 mm which implies an origin in disks of size of size about 13 AU and mass about 0.024 solar mass. The 2.6 mm emission of the GG Tau system, a hierarchical quadrupole, is partially resolved. Strong emission extended over about 3 x 5 arcsec is associated with the close binary GG Tau. Weak emission is detected at GG Tau/c, also a close binary. Evidently extensive dusty disks can survive in the environment of close binaries for at least about 10 exp 5 yr, and their structure can vary markedly from system to system.

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