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 \farcs 1 ( \sim 5 AU ) and 1 \farcs 0 ( \sim 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 ) \propto r ^ { -0.5 } and \Sigma ( r ) \propto r ^ { -1 } .
These properties are consistent with an irradiated gaseous accretion disk of mass \sim 0.03 ~ { } { M _ { \odot } } with an accretion rate \sim 10 ^ { -8 } ~ { } { M _ { \odot } ~ { } 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 .