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Recently, the CO J=3-2 observational result of the envelope of the 21micrometer PPN IRAS 07134+1005 has been reported. Assuming that the CO J=3-2line was optically thin, the mass-loss rate of the superwind in this PPN wasfound to be at least 2 orders of magnitude lower than the typical range. Inorder to obtain a more accurate mass-loss rate, we reexamine this data andconstruct a radiative transfer model to compare with the data. Also, in orderto better resolve the superwind, we adopt a different weighting on the data toobtain maps at higher resolution. Our result shows that the CO J=3-2 emissionis located slightly further away from the central source than the mid-IRemission, probably because that the material is cooler in the outer part andthus better traced by the CO emission. At lower resolution, however, the COemission appeared to be spatially coincident with the mid-IR emission. Ourmodel has two components, an inner ellipsoidal shell-like superwind with anequatorial density enhancement and an outer spheroidal AGB wind. The thicktorus in previous model could be considered as the dense equatorial part of ourellipsoidal superwind. With radiative transfer, our model reproduces moreobserved features than previous model and obtains an averaged superwindmass-loss rate of ~ 1.8 x 10^-5 solar mass per year, which is typical for asuperwind. The mass-loss rate in the equatorial plane is 3 x 10^-5 solar massper year, also the same as that derived before from modeling CO J=1-0 emission.

Remodel the Envelope Around the 21 micrometer PPN IRAS 07134+1005