We model multi-wavelength broadband UBVIJHK _ { s } 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 . ( 75 ) and a “ KMH ” -like grain size distribution with \gamma of -3.5 , a _ { min } of 0.01 { \mu m } , and a _ { 0 } of 0.1 { \mu m } 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 . Our models of the data require the luminosity of SSTSAGE052206 and HV 5715 to be { \sim } 5 100 L _ { \sun } and { \sim } 36 000 L _ { \sun } , respectively . This , combined with the stellar effective temperatures of 3 700 K and 3 500 K , respectively , that we find best fit the optical and near-infrared data , suggests stellar masses of { \sim } 3 M _ { \sun } and { \sim } 7 M _ { \sun } . This , in turn , suggests that HV 5715 is undergoing hot bottom burning and that SSTSAGE052206 is not . Our models of SSTSAGE052206 and HV 5715 require dust shells of inner radius { \sim } 17 and { \sim } 52 times the stellar radius , respectively , with dust temperatures there of 900 K and 430 K , respectively , and with optical depths at 10 { \mu m } through the shells of 0.095 and 0.012 , respectively . The models compute the dust mass-loss rates for the two stars to be 2.0 \times 10 ^ { -9 } { \it M _ { \odot } } yr ^ { -1 } and 2.3 \times 10 ^ { -9 } { \it M _ { \odot } } yr ^ { -1 } , 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 1.0 \times 10 ^ { -6 } { \it M _ { \odot } } yr ^ { -1 } and 1.2 \times 10 ^ { -6 } { \it M _ { \odot } } yr ^ { -1 } , 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 .