THE DYNAMICALLY DISRUPTED GAP IN HD 142527

被引:74
作者
Casassus, S. [1 ,8 ]
Perez, S. M. [1 ,8 ]
Jordan, A. [2 ,8 ]
Menard, F. [1 ,3 ,4 ,8 ]
Cuadra, J. [2 ]
Schreiber, M. R. [5 ,8 ]
Hales, A. S. [6 ,8 ]
Ercolano, B. [7 ]
机构
[1] Univ Chile, Dept Astron, Santiago, Chile
[2] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile
[3] CNRS INSU, UMI FCA 3386, Santiago, Chile
[4] CNRS UJF UMR 5274, IPAG, Grenoble, France
[5] Univ Valparaiso, Dept Fis & Astron, Valparaiso, Chile
[6] Joint ALMA Observ, Santiago 7630355, Chile
[7] Univ Munich, Univ Observ, Munich, Germany
[8] Univ Chile, Millenium Nucleus Protoplanetary Disks ALMA Early, Santiago, Chile
关键词
planet-disk interactions; protoplanetary disks; stars: individual (HD 142527); stars: pre-main sequence; DISK SURROUNDING HD-142527; HERBIG AE STARS; PROTOPLANETARY DISK; PLANET; SYSTEMS; YOUNG; EVOLUTION; COMPANION; AURIGAE; IMAGES;
D O I
10.1088/2041-8205/754/2/L31
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The vestiges of planet formation have been observed in debris disks harboring young and massive gaseous giants. The process of giant planet formation is terminated by the dissipation of gas in the protoplanetary disk. The gas-rich disk around HD 142527 features a small inner disk, a large gap from similar to 10 to similar to 140 AU, and a massive outer disk extending out to similar to 300 AU. The gap could have been carved out by a giant planet. We have imaged the outer regions of this gap using the adaptive optics camera NICI on Gemini South. Our images reveal that the disk is dynamically perturbed. The outer boundary of the roughly elliptical gap appears to be composed of several segments of spiral arms. The stellar position is offset by 0 ''.17 +/- 0 ''.02 from the centroid of the cavity, consistent with earlier imaging at coarser resolutions. These transient morphological features are expected in the context of disk evolution in the presence of a perturbing body located inside the cavity. We perform hydrodynamical simulations of the dynamical clearing of a gap in a disk. A 10 M-jup body in a circular orbit at r = 90 AU perturbs the whole disks, even after thousands of orbits. By then the model disk has an eccentric and irregular cavity, flanked by tightly wound spiral arms, but it is still evolving far from steady state. A particular transient configuration that is a qualitative match to HD 142527 is seen at 1.7 Myr.
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页数:5
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