Keck/NIRC2 Imaging of the Warped, Asymmetric Debris Disk around HD 32297
Thayne Currie, Timothy J. Rodigas, John Debes, Peter Plavchan, Marc Kuchner, Hannah Jang-Condell, David Wilner, Sean Andrews, Adam Kraus, Scott Dahm, Thomas Robitaille
备注：
19 pages, 12 figures; ApJ in press (no text changes from previous version)
We present Keck/NIRC2 $K_{s}$ band high-contrast coronagraphic imaging of the luminous debris disk around the nearby, young A star HD 32297 resolved at a projected separation of $r$ = 0.3-2.5\arcsec{} ($\approx$ 35-280 AU). The disk is highly warped to the north and exhibits a complex, "wavy" surface brightness profile interior to $r$ $\approx$ 110 AU, where the peaks/plateaus in the profiles are shifted between the NE and SW disk lobes. The SW side of the disk is 50--100% brighter at $r$ = 35-80 AU, and the location of its peak brightness roughly coincides with the disk's mm emission peak. Spectral energy distribution modeling suggests that HD 32297 has at least two dust populations that may originate from two separate belts likely at different locations, possibly at distances coinciding with the surface brightness peaks. A disk model for a single dust belt including a phase function with two components and a 5-10 AU pericenter offset explains the disk's warped structure and reproduces some of the surface brightness profile's shape (e.g. the overall "wavy" profile, the SB peak/plateau shifts) but more poorly reproduces the disk's brightness asymmetry. Although there may be alternate explanations, agreement between the SW disk brightness peak and disk's peak mm emission is consistent with an overdensity of very small, sub-blowout-sized dust and large, 0.1-1 mm-sized grains at $\approx$ 45 AU tracing the same parent population of planetesimals. New near-IR and submm observations may be able to clarify whether even more complex grain scattering properties or dynamical sculpting by an unseen planet are required to explain HD 32297's disk structure.
Formation History of HD106906 and the Vertical Warping of Debris Disks by an External Inclined Companion
HD 106906是一个行星系，拥有一个宽轨道的伴星，以及一个偏心和扁平的碎片盘，这对它的形成和随后的演变有重要的限制。最近对伴星的观测表明，它的轨道是偏心的，相对于碎片盘的平面倾斜。在这里，我们表明，在倾斜的同伴的存在下，碎片盘迅速（$\lesssim5$ Myr）变得扭曲和膨胀。这表明该系统的当前配置是相对较新的。我们探讨了最近与自由浮动行星的近距离接触可能产生轨道参数与HD106906b观测一致的伴星的可能性。我们发现，这种情况下是能够重建的碎片盘的结构，同时产生一个同伴与观察一致。
The multi-wavelength vertical structure of the archetypal $β$ Pictoris debris disk
California Institute of Technology（加州理工学院）；University of Cambridge（剑桥大学）；University of Belgrade（贝尔格莱德大学）；University of Oxford（牛津大学）；ALMA JAO（阿塔卡马大型毫米波/亚毫米波阵列联合运营办公室）；Wesleyan University（卫斯理安大学）；Trinity College Dublin, the University of Dublin（都柏林三一学院，都柏林大学）
Deep HST/STIS Coronagraphic Imaging of the $β$ Pictoris Debris Disk: On the Scattered Light Component of the Cat's Tail
The University of Arizona（亚利桑那大学）；Centro de Astrobiología (CAB, CSIC-INTA)（天体生物学中心（CAB，CSIC-INTA））；Space Telescope Science Institute（太空望远镜科学研究所）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）
