2013A&A...560A.105G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.12CEST09:51:47

2013A&A...560A.105G - Astronomy and Astrophysics, volume 560A, 105-105 (2013/12-1)

Small vs. large dust grains in transitional disks: do different cavity sizes indicate a planet? SAO 206462 (HD 135344B) in polarized light with VLT/NACO.

GARUFI A., QUANZ S.P., AVENHAUS H., BUENZLI E., DOMINIK C., MERU F., MEYER M.R., PINILLA P., SCHMID H.M. and WOLF S.

Abstract (from CDS):

Transitional disks represent a short stage of the evolution of circumstellar material. Studies of dust grains in these objects can provide pivotal information on the mechanisms of planet formation. Dissimilarities in the spatial distribution of small (µm-size) and large (mm-size) dust grains have recently been pointed out. Constraints on the small dust grains can be obtained by imaging the distribution of scattered light at near-infrared wavelengths. We aim at resolving structures in the surface layer of transitional disks (with particular emphasis on the inner 10-50 AU), thus increasing the scarce sample of high-resolution images of these objects. We obtained VLT/NACO near-IR high-resolution polarimetric differential imaging observations of SAO 206462 (HD135344B). This technique allows one to image the polarized scattered light from the disk without any occulting mask and to reach an inner working angle of ∼0.1". A face-on disk is detected in H and Ks bands between 0.1" and 0.9". No significant differences are seen between the H and Ks images. In addition to the spiral arms, these new data allow us to resolve for the first time an inner disk cavity for small dust grains. The cavity size (≃28AU) is much smaller than what is inferred for large dust grains from (sub-)mm observations (39 to 50AU). This discrepancy cannot be ascribed to any resolution effect. The interaction between the disk and potential orbiting companion(s) can explain both the spiral arm structure and the discrepant cavity sizes for small and large dust grains. One planet may be carving out the gas (and, thus, the small grains) at 28AU, and generating a pressure bump at larger radii (39AU), which holds back the large grains. We analytically estimate that, in this scenario, a single giant planet (with a mass between 5 and 15MJ) at 17 to 20AU from the star is consistent with the observed cavity sizes.

Abstract Copyright:

Journal keyword(s): stars: pre-main sequence - protoplanetary disks - ISM: individual objects: SAO 206462 - techniques: polarimetric

VizieR on-line data: <Available at CDS (J/A+A/560/A105): list.dat fits/*>

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* UX Tau A TT* 04 30 03.9931880444 +18 13 49.476948664   12.92 11.15     K2Ve 327 0
2 V* UX Tau Or* 04 30 03.99626 +18 13 49.4355 11.23 11.84 10.80 9.83 9.05 K2Ve+M1Ve 311 0
3 V* V1213 Tau Or* 04 31 37.47192 +18 12 24.4800           K7 516 0
4 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 552 0
5 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 932 2
6 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 394 0
7 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 358 0
8 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 651 1
9 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 357 1
10 HD 135344 * 15 15 48.9457954324 -37 08 55.727525343   7.84 7.76     A0V 128 1
11 Ass Sco OB 2-3 * 15 49.7 -26 59           ~ 15 0
12 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 467 1
13 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 233 1
14 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 335 2

    Equat.    Gal    SGal    Ecl

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2020.07.12-09:51:47

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