Dusty disks in the multiple systems UZ Tauri and GG Tauri
Citations Over TimeTop 10% of 1992 papers
Abstract
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.
Related Papers
- Forbidden emission lines in Herbig Ae/Be stars ?(1997)
- → Do Herbig Ae/Be Stars Have Disks?(1997)1 cited
- Magnetic structure in cool stars. XVIII : UV-line emissions from T Tauri stars(1992)
- → The X-Ray Emission of T Tauri Stars in Taurus-Auriga as Seen from the Einstein Observatory IPC(1993)
- → Forbidden line emission and correlations with the infra-red excess in Herbig Ae/Be stars(1996)