  To measure the mass loss from dusty oxygen-rich (O-rich) evolved stars in the
Large Magellanic Cloud (LMC), we have constructed a grid of models of
spherically-symmetric dust shells around stars with constant mass-loss rates
using 2Dust. These models will constitute the O-rich model part of the "Grid of
Red supergiant and Asymptotic giant branch star ModelS" (GRAMS). This model
grid explores 4 parameters - stellar effective temperature from 2100 K - 4700
K; luminosity from 10^3-10^6 L_Sun; dust shell inner radii of 3, 7, 11, and 15
R_Star; and 10.0 micron optical depth from 10^-4 to 26. From an initial grid of
~1200 2Dust models, we create a larger grid of ~69,000 models by scaling to
cover the luminosity range required by the data. These models are offered to
the public on a website. The matching in color-magnitude diagrams and
color-color diagrams to observed O-rich asymptotic giant branch (AGB) and red
supergiant (RSG) candidate stars from the SAGE and SAGE-Spec LMC samples and a
small sample of OH/IR stars is generally very good. The extreme AGB star
candidates from SAGE are more consistent with carbon-rich (C-rich) than O-rich
dust composition. Our model grid suggests lower limits to the mid-infrared
colors of the dustiest AGB stars for which the chemistry could be O-rich.
Finally, the fitting of GRAMS models to SEDs of sources fit by other studies
provides additional verification of our grid and anticipates future, more
expansive efforts.
