The TW Hya system is perhaps the closest analog to the early solar nebula. We have used the Very Large Array to image TW Hya at wavelengths of 7 mm and 3.6 cm with resolutions 0.′′1 (~5 AU) and 1.′′0 (~50 AU), respectively. The 7 mm emission is extended and appears dominated by a dusty disk of radius >50 AU surrounding the star. The 3.6 cm emission is unresolved and likely arises from an ionized wind or gyrosynchrotron activity. The dust spectrum and spatially resolved 7 mm images of the TW Hya disk are fitted by a simple model with temperature and surface density described by radial power laws, T(r)(alpha)r^−0.5 and Sigma(r)(alpha) r^−1. These properties are consistent with an irradiated gaseous accretion disk of mass ~0.03 M⊙ with an accretion rate ~10−^8 M⊙ yr^−1 and viscosity parameter alpha= 0.01. The estimates of mass and mass accretion rates are uncertain as the gas-to-dust ratio in the TW Hya disk may have evolved from the standard interstellar value (Refer to PDF file for exact formulas).
Department, Program, or Center
Chester F. Carlson Center for Imaging Science (COS)
Astrophys.J.L. 534 (2000) L101-L104
RIT – Main Campus