Wavelength-dependent far-infrared polarization of HL Tau observed with SOFIA/HAWC+

Abstract

We present the first polarimetric observations of a circumstellar disk in the far-infrared wavelength range. We report flux and linear polarization measurements of the young stellar object HL Tau in the bands A (53 $\mu$m), C (89 $\mu$m), D (155 $\mu$m), and E (216 $\mu$m) with SOFIA/HAWC+. The orientation of the polarization vectors is strongly wavelength-dependent and can be attributed to different wavelength-dependent polarization mechanisms in the disk and its local environment. In bands A, C, and D, the orientation of the polarization is roughly consistent with a value of 114° at the maximum emission. Hereby, the magnetic field direction is close to that of the spin axis of the disk. In contrast, in band E, the orientation is nearly parallel to the minor axis of the projection of the inclined disk. Based on a viscous accretion disk model combined with a surrounding envelope, we performed polarized three-dimensional Monte Carlo radiative transfer simulations. In particular, we considered polarization due to emission and absorption by aligned dust grains, and polarization due to scattering of the thermal reemission (self-scattering). At wavelengths of 53 $\mu$m, 89 $\mu$m, and 155 $\mu$m, we were able to reproduce the observed orientation of the polarization vectors. Here, the origin of polarization is consistent with polarized emission by aligned non-spherical dust grains. In contrast, at a wavelength of 216 $\mu$m, the polarization pattern could not be fully matched, however, applying self-scattering and assuming dust grain radii up to 35 $\mu$m, we were able to reproduce the flip in the orientation of polarization. We conclude that the polarization is caused by dichroic emission of aligned dust grains in the envelope, while at longer wavelengths, the envelope becomes transparent and the polarization is dominated by self-scattering in the disk.

11 pages, 6 figures, to be published in Astronomy & Astrophysics (A&A), updated URL to IRSA

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