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tokens: ( 2003 ), the polarization degree of the dust emission 6 is expected to be a few to 10 percent for a typical line of sight at an angle 45 o with respect to the magnetic field (Lee Draine 1985 ). Similar to the polarimetry of IR emission from AGN torus (e.g. Packham et al. 2007 ; Lopez-Rodriguez et al. 2013 ), future IR polarimetry of TDEs could potentially play an important role in studying the dust properties and magnetic field around non-AGN. 4.2 Possible refinements of the model A few other complexities, which are ignored in our simple model, can be taken into account in future works. (1) The heating by the scattered UV-optical photons and dust IR radiation could be included by considering the time delay and related absorption coefficient. In this way, a spectrum of dust IR emission can be calculated and compared with future observations. (2) The clumpiness of dusty clouds will affect the radiative transfer. Since every clump will have a bright (hot) side and a dark (cold) side, dust temperature distributions are different in clumpy and smooth environments (Nenkova et al. 2008 ). (3) In the radiative transfer model in Section 3 , a single dust radius of a = 0.1 μm is used, but the true interstellar grain population has a broad size distribution, extending from a few Å (PAH molecules) to about 0.2 μm (or even larger). Most mass is in the larger grains, with half-mass grain radius typically ∼ 0.1 μm (half of mass is in grains with radius above this value), and the smaller grains contribute most surface area and hence most UV extinction (e.g. Laor Draine 1993 ; Weingartner Draine 2001 ). However, at the same distance from the central source, smaller grains sublime faster than larger ones (mostly due to higher grain temperatures), so it is unclear which grain size contributes most IR emission. Also, the properties of graphite and silicate grains are sufficiently different that their sublimation radii could be separated. A systematic study of grain size distribution and chemical composition could be done in the future with dust continuum radiative transfer codes such as DUSTY 7 and HYPERION, 8 although the dynamical propagation of radiation coupled with dust sublimation requires some modification of the codes. 5 SUMMARY We consider the impact of the UV-optical radiation ( E rad ∼ 10 51 –10 52 erg) from TDEs on the circum-nuclear medium. If the medium is dusty, the UV-optical radiation energy will be absorbed by dust within ∼1 pc from the BH and re-radiated in the IR. We calculate the bolometric light-curve from a 1D radiative transfer model, taking into account the time-dependent heating, cooling and sublimation of dust grains. We show that the dust emission peaks at 3-10 μm and has typical luminosities between 10 42 and 10 43 erg s −1 (with sky covering factor f Ω ranging from 0.1 to 1). This is detectable by current generation of ground-based and space telescopes. In the near future, JWST will be able to perform photometric and