  We model multi-wavelength broadband UBVIJHKs and Spitzer IRAC and MIPS
photometry and IRS spectra from the SAGE and SAGE-Spec observing programs of
two oxygen-rich asymptotic giant branch (O-rich AGB) stars in the Large
Magellanic Cloud (LMC) using radiative transfer models of dust shells around
stars. We chose a star from each of the bright and faint O-rich AGB populations
found by earlier studies of the SAGE sample in order to derive a baseline set
of dust properties to be used in the construction of an extensive grid of
radiative transfer models of the O-rich AGB stars found in the SAGE surveys.
From the bright O-rich AGB population we chose HV 5715, and from the faint
O-rich AGB population we chose SSTISAGE1C J052206.92-715017.6 (SSTSAGE052206).
We found the complex indices of refraction of oxygen-deficient silicates from
Ossenkopf et al (1992) and a "KMH"-like grain size distribution with gamma of
-3.5, a_min of 0.01 microns, and a_0 of 0.1 microns to be reasonable dust
properties for these models. There is a slight indication that the dust around
the faint O-rich AGB may be more silica-rich than that around the bright O-rich
AGB. Simple models of gas emission suggest a relatively extended gas envelope
for the faint O-rich AGB star modeled, consistent with the relatively large
dust shell inner radius for the same model. The models compute the dust
mass-loss rates for the two stars to be 2.0x10^-9 M_Sun/yr and 2.3x10^-9
M_Sun/yr, respectively. When a dust-to-gas mass ratio of 0.002 is assumed for
SSTSAGE052206 and HV 5715, the dust mass-loss rates imply total mass-loss rates
of 1.0x10^-6 M_Sun/yr and 1.2x10^-6 M_Sun/yr, respectively. These properties of
the dust shells and stars, as inferred from our models of the two stars, are
found to be consistent with properties observed or assumed by detailed studies
of other O-rich AGB stars in the LMC and elsewhere.
