期刊
ASTROPHYSICAL JOURNAL LETTERS
卷 748, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/748/2/L22
关键词
circumstellar matter; instrumentation: high angular resolution; polarization; protoplanetary disks; stars: individual (SAO 206462, HD 135344B); waves
资金
- KAKENHI [22000005, 23103002, 23103004, 23103005, 23244027, 18540238, 22.2942]
- WPI Initiative, MEXT, Japan
- NSF AST [1008440, 1009203, 1009314]
- NASA [NNH06CC28C, NNX09AC73G]
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [0901967, 1009314] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1008440, 1009203] Funding Source: National Science Foundation
- Grants-in-Aid for Scientific Research [22000005, 23103001, 23244027, 21244022, 23740151, 20540232, 24840037, 23103004] Funding Source: KAKEN
- NASA [NNX09AC73G, 120162] Funding Source: Federal RePORTER
We present high-resolution, H-band imaging observations, collected with Subaru/HiCIAO, of the scattered light from the transitional disk around SAO 206462 (HD 135344B). Although previous sub-mm imagery suggested the existence of a dust-depleted cavity at r <= 46 AU, our observations reveal the presence of scattered light components as close as 0 ''.2 (similar to 28 AU) from the star. Moreover, we have discovered two small-scale spiral structures lying within 0.'' 5 (similar to 70 AU). We present models for the spiral structures using the spiral density wave theory, and derive a disk aspect ratio of h similar to 0.1, which is consistent with previous sub-mm observations. This model can potentially give estimates of the temperature and rotation profiles of the disk based on dynamical processes, independently from sub-mm observations. It also predicts the evolution of the spiral structures, which can be observable on timescales of 10-20 years, providing conclusive tests of the model. While we cannot uniquely identify the origin of these spirals, planets embedded in the disk may be capable of exciting the observed morphology. Assuming that this is the case, we can make predictions on the locations and, possibly, the masses of the unseen planets. Such planets may be detected by future multi-wavelength observations.
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