GAPS IN THE HD 169142 PROTOPLANETARY DISK REVEALED BY POLARIMETRIC IMAGING: SIGNS OF ONGOING PLANET FORMATION?
GAPS IN THE HD 169142 PROTOPLANETARY DISK REVEALED BY POLARIMETRIC IMAGING: SIGNS OF ONGOING PLANET FORMATION?
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偏振成像揭示的 HD 169142 原行星盘中的间隙：正在进行的行星形成的迹象？
DOI：
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
S. Wolf
中科院分区：
文献类型：
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作者：
S. Quanz;H. Avenhaus;E. Buenzli;A. Garufi;H. Schmid;S. Wolf
我们展示了赫比格Ae/Be星星HD 169142的H波段甚大望远镜/纳科偏振光图像，探测其原行星盘，距离星星约为1.00.“1。我们的图像追踪到了盘面的101.″7（10250 Au），并首次揭示了不同的亚结构：（1）内盘（1020 Au）似乎被散射的尘埃颗粒耗尽;（2）在1025 Au处成像到了一个未分辨的盘边缘;（3）环形间隙从1040延伸到70 Au;（4）在环形间隙的相对侧上发现局部亮度不对称。我们讨论了观察到的形态，其中正在进行的行星形成是一个诱人的，但尚未被证明，一个不同的解释。在85 Au以外，表面亮度大约下降到Δ r−3.3，但分别用幂律Δ r−2.6和Δ r−3.9描述85-120 Au和120-250 Au之间的盘区域，可以提供更好的拟合，暗示盘表面的另一个不连续性。圆盘积分的偏振光和中心星星之间的通量比为10.4.1 × 10−3。最后，将我们的结果与文献中的结果相结合，发现H带中约40%的散射光是偏振的。我们的研究结果强调，HD 169142是未来行星形成或磁盘演化研究的一个有趣的系统。
We present H-band Very Large Telescope/NACO polarized light images of the Herbig Ae/Be star HD 169142 probing its protoplanetary disk as close as ∼0.″1 to the star. Our images trace the face-on disk out to ∼1.″7 (∼250 AU) and reveal distinct substructures for the first time: (1) the inner disk (≲20 AU) appears to be depleted in scattering dust grains; (2) an unresolved disk rim is imaged at ∼25 AU; (3) an annular gap extends from ∼40 to 70 AU; (4) local brightness asymmetries are found on opposite sides of the annular gap. We discuss different explanations for the observed morphology among which ongoing planet formation is a tempting, but yet to be proven, one. Outside of ∼85 AU the surface brightness drops off roughly ∝r−3.3, but describing the disk regions between 85–120 AU and 120–250 AU separately with power laws ∝r−2.6 and ∝r−3.9 provides a better fit hinting toward another discontinuity in the disk surface. The flux ratio between the disk-integrated polarized light and the central star is ∼4.1 × 10−3. Finally, combining our results with those from the literature, ∼40% of the scattered light in the H band appears to be polarized. Our results emphasize that HD 169142 is an interesting system for future planet formation or disk evolution studies.
影响因子：
6.5
作者：
J. P. Ruge;S. Wolf;A. Uribe;H. Klahr
通讯作者：
J. P. Ruge;S. Wolf;A. Uribe;H. Klahr