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Polarized continuum emission from aligned grains in disks around youngstellar objects can be used to probe the magnetic field, radiation anisotropy,or drift between dust and gas, depending on whether the non-spherical grainsare aligned magnetically, radiatively or mechanically. We show that it can alsobe used to probe another key disk property -- the temperature gradient -- alongsight lines that are optically thick, independent of the grain alignmentmechanism. We first illustrate the technique analytically using a simple 1Dslab model, which yields an approximate formula that relates the polarizationfraction to the temperature gradient with respect to the optical depth tau atthe tau=1 surface. The formula is then validated using models of stellarirradiated disks with and without accretion heating. The promises andchallenges of the technique are illustrated with a number of Class 0 and Idisks with ALMA dust polarization data, including NGC 1333 IRAS4A1, IRAS16293B, BHB 07-11, L1527, HH 212 and HH 111. We find, in particular, that thesight lines passing through the near-side of a highly inclined disk tracedifferent temperature gradient directions than those through the far-side,which can lead to a polarization orientation on the near-side that isorthogonal to that on the far-side, and that the HH 111 disk may be such acase. Our technique for probing the disk temperature gradient through dustpolarization can complement other methods, particularly those using molecularlines.

Probing the Temperature Structure of Optically Thick Disks Using Polarized Emission of Aligned Grains