2011A&A...529A.105G


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.03CEST22:47:51

2011A&A...529A.105G - Astronomy and Astrophysics, volume 529A, 105-105 (2011/5-1)

A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties.

GUILLOTEAU S., DUTREY A., PIETU V. and BOEHLER Y.

Abstract (from CDS):

Proto-planetary disks are thought to provide the initial environment for planetary system formation. The dust and gas distribution and its evolution with time is one of the key elements in the process. We attempt to characterize the radial distribution of dust in disks around a sample of young stars from an observational point of view, and, when possible, in a model-independent way, by using parametric laws. We used the IRAM PdBI interferometer to provide very high angular resolution (down to 0.4'' in some sources) observations of the continuum at 1.3 mm and 3 mm around a sample of T Tauri stars in the Taurus-Auriga region. The sample includes single and multiple systems, with a total of 23 individual disks. We used track-sharing observing mode to minimize the biases. We fitted these data with two kinds of models: a ``truncated power law'' model and a model presenting an exponential decay at the disk edge (``viscous'' model). Direct evidence for tidal truncation is found in the multiple systems. The temperature of the mm-emitting dust is constrained in a few systems. Unambiguous evidence for large grains is obtained by resolving out disks with very low values of the dust emissivity index β. In most disks that are sufficiently resolved at two different wavelengths, we find a radial dependence of β, which appears to increase from low values (as low as 0) at the center to about 1.7-2 at the disk edge. The same behavior could apply to all studied disks. It introduces further ambiguities in interpreting the brightness profile, because the regions with apparent β≃0 can also be interpreted as being optically thick when their brightness temperature is high enough. Despite the added uncertainty on the dust absorption coefficient, the characteristic size of the disk appears to increase with a higher estimated star age. These results provide the first direct evidence of the radial dependence of the grain size in proto-planetary disks. Constraints of the surface density distributions and their evolution remain ambiguous because of a degeneracy with the β(r) law.

Abstract Copyright:

Journal keyword(s): protoplanetary disks - stars: formation - planetary systems - dust, extinction

Simbad objects: 31

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Number of rows : 31

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* CY Tau Or* 04 17 33.7281514373 +28 20 46.809969664 14.52 14.68 13.40 12.59   M1.5 229 0
2 V* BP Tau Or* 04 19 15.8342975037 +29 06 26.929456808   13.13 12.12 11.89   K5/7Ve 599 0
3 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 648 1
4 V* T Tau Or* 04 21 59.4323326335 +19 32 06.439974179   11.01 9.30 9.80   K0IV/Ve 1249 2
5 NAME T Tau N *i* 04 21 59.433 +19 32 06.42   11.22 10.12 9.80   K1.5 164 1
6 V* FT Tau Or* 04 23 39.1894939930 +24 56 14.248383831   16.15 14.93 14.70   M2.8 109 0
7 2MASS J04270266+2605304 Y*O 04 27 02.66593 +26 05 30.3790           ~ 135 0
8 V* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
9 V* GV Tau TT* 04 29 23.7314759229 +24 33 00.216016292 19.20         K7 271 2
10 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1216 0
11 V* V1213 Tau Or* 04 31 37.47192 +18 12 24.4800           K7 516 0
12 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1201 0
13 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
14 Haro 6-13 Or* 04 32 15.4177438039 +24 28 59.580866027 19.22   17.7     M0 181 1
15 V* GG Tau Or* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 647 1
16 V* UZ Tau B TT* 04 32 42.82968 +25 52 31.4148   14.07 12.72 13.35   M1/3Ve 136 0
17 V* UZ Tau ** 04 32 43.02168 +25 52 30.9036           M4Ve+M1/3Ve 285 0
18 V* UZ Tau A TT* 04 32 43.0744163742 +25 52 31.022242441       13.15   M2.0e+M3.0e 88 0
19 V* DL Tau Or* 04 33 39.0766866461 +25 20 38.097973550 14.04 14.59 13.40 11.85 10.89 K7Ve 282 0
20 V* DM Tau Or* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 510 0
21 V* CI Tau Or* 04 33 52.0144455735 +22 50 30.093741884 14.97 15.09 13.80     K4IVe 261 1
22 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 552 1
23 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
24 Haro 6-33 TT* 04 41 38.8300758211 +25 56 26.681998749     18.40     M0.5 100 2
25 V* DQ Tau Or* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 286 0
26 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 552 0
27 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 930 2
28 HD 31648 Ae* 04 58 46.2654165113 +29 50 36.990341242 7.84 7.78 7.62 7.76 7.43 A5Vep 394 0
29 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 358 0
30 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 255 0
31 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 707 0

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2020.07.03-22:47:51

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