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We conduct a systematic examination of the properties of models forchemically homogeneous, differentially rotating, main-sequence stars of mass1-2 M_sun. The models were constructed using a code based on a reformulation ofthe self-consistent field method of computing the equilibrium stellar structurefor a specified conservative internal rotation law. [abridged] Relative tononrotating stars of the same mass, these models all have reduced luminositiesand effective temperatures, and flattened photospheric shapes (i.e., decreasedpolar radii) with equatorial radii that can be larger or smaller, depending onthe degree of differential rotation. For a fixed ratio of the axial rotationrate to the surface equatorial rotation rate, increasingly rapid rotationgenerally deepens convective envelopes, shrinks convective cores, and can leadto the presence of a convective core (envelope) in a 1 M_sun (2 M_sun) model, afeature that is absent in a nonrotating star of the same mass. The positions ofdifferentially rotating models for a given mass M in the H-R diagram can beshifted in such a way as to approximate the nonrotating ZAMS over ranges inluminosity and effective temperature that correspond to a mass interval betweenM and about 0.7 M. We briefly note a few of the implications of these results,including (i) possible ambiguities arising from similarities between theproperties of rotating and nonrotating models of different masses, (ii) areduced radiative luminosity for a young, rapidly rotating Sun, (iii) thenuclear destruction of lithium and other light metallic species in the layersbeneath an outer convective envelope, and (iv), the excitation of solar-likeoscillations and the operation of a solar-like hydromagnetic dynamo in some1.5-2 M_sun stars.

On the Structure and Properties of Differentially Rotating Main-Sequence Stars in the 1-2 M_sun Range