Stellar radius evolution for 1- and 0.3-M_⊙stars predicted by the Dartmouth standard model (Dotter 2016), the Dartmouth magnetic model , which includes the inflationary effect of magnetic fields via spots and inhibition of convection (Feiden 2016), and the Baraffe et al. (2015) model. In the Dartmouth models a different set of abundances and opacities results in prolonged deuterium burning compared to the Baraffe et al. (2015) model (G. Feiden, pers. comm.). This delays stellar contraction and potential affects disk evolution via the radius dependence of Eqn. 4.