摘要：We present the first polarimetric detection of the inner disk component around the pre-main-sequence B9.5 star HD 141569A.Gemini Planet Imager H-band (1.65 μm) polarimetric differential imaging reveals the highest signal-to-noise ratio detection of this ring yet attained and traces structure inward to 0farcs25 (28 au at a distance of 111 pc).The radial polarized intensity image shows the east side of the disk, peaking in intensity at 0farcs40 (44 au) and extending out to 0farcs9 (100 au).There is a spiral arm–like enhancement to the south, reminiscent of the known spiral structures on the outer rings of the disk.The location of the spiral arm is coincident with 12CO J = 3–2 emission detected by ALMA and hints at a dynamically active inner circumstellar region.Our observations also show a portion of the middle dusty ring at ~220 au known from previous observations of this system.We fit the polarized H-band emission with a continuum radiative transfer Mie model.Our best-fit model favors an optically thin disk with a minimum dust grain size close to the blowout size for this system, evidence of ongoing dust production in the inner reaches of the disk.The thermal emission from this model accounts for virtually all of the far-infrared and millimeter flux from the entire HD 141569A disk, in agreement with the lack of ALMA continuum and CO emission beyond ~100 au.A remaining 8–30 μm thermal excess a factor of ~2 above our model argues for an as-yet-unresolved warm innermost 5–15 au component of the disk.
