The Roles of Dust Growth in the Temperature Evolution and Snow Line Migration in Magnetically Accreting Protoplanetary Disks

The temperature structure of protoplanetary disks provides an important constraint on where in the rocky planets like our own form. Recent nonideal magnetohydrodynamical (MHD) simulations have shown that internal Joule heating associated with magnetically driven disk accretion is inefficient at midplane. A model based MHD predicts a around solar-mass young star, water snow line can move inside current Earth's orbit within 1 Myr after formation. However, efficiency depends disk's ionization and opacity structures, both which are governed by dust grains. In this study, we investigate these effects combing previous for accreting parameterized grain size vertical distribution. Grain growth enhances gas fraction thereby allows to occur closer beyond 10 $\rm \mu m$ causes decrease opacity, leading lower midplane temperature. combination two results being maximized when range 10-100 m$. millimeter sizes also delay line's migration au up few Myr. We conclude accounting essential accurately modeling evolution terrestrial planet formation disks.