2010A&A...512A..15R


C.D.S. - SIMBAD4 rel 1.7 - 2021.01.26CET01:38:50

2010A&A...512A..15R - Astronomy and Astrophysics, volume 512, A15-15 (2010/3-1)

Dust properties of protoplanetary disks in the Taurus-Auriga star forming region from millimeter wavelengths.

RICCI L., TESTI L., NATTA A., NERI R., CABRIT S. and HERCZEG G.J.

Abstract (from CDS):

We present the most sensitive 3mm-survey to date of protoplanetary disks carried out in the Taurus-Auriga star forming region (average rms of about 0.3mJy), using the IRAM PdBI. With our high detection rate of 17/19 we provide the first detections at wavelengths longer than about 1 mm for 12 sources. This enables us to statistically study the mm SED slopes and dust properties of faint disks and compare them to brighter disks using a uniform analysis method. With these new data and literature measurements at sub-millimeter and millimeter wavelengths, we analyze the dust properties of a sample of 21 isolated disks around T Tauri stars in the Taurus-Auriga star forming region. Together with the information about the disks' spatial extension from sub/mm-mm interferometric studies, we derive from the observed sub-mm/mm spectral energy distribution constraints on the dust opacity law at these wavelengths, using two-layer flared disk models and a self-consistent dust model that properly takes into account the variation of the dust opacity with grain growth. We find evidence for the presence of dust particles in the disk midplane that have grown to sizes as large as at least 1 millimeter in all the disks of our sample, confirming what was previously observed on smaller brighter objects. This indicates that the dust coagulation from ISM dust to mm-sized grains is a very fast process in protoplanetary disks, which appears to occur before a young stellar object enters the class II evolutionary stage. The amount of these large grains in the disk outer regions is also found to be stationary throughout the whole class II evolutionary stage, which indicates that mechanisms slowing down the dust inward migration play an important role in the Taurus-Auriga protoplanetary disks. Another result is that the spectral index between 1 and 3mm for the six faintest disks in our sample is on average smaller than for the brighter disks, indicating either that these fainter yet unmapped disks are spatially much less extended than the brighter spatially resolved disks, or that fainter disks have typically larger dust grains in their outer regions. Considering that these fainter disks are more representative of the bulk of the disk population than the brighter ones, this may have important consequences for the theories of planetesimal formation and disk formation and evolution. Finally, we investigate the relations between the derived dust properties, namely dust mass and grain growth, and the properties of the central star, like its mass, age and mass accretion rate.

Abstract Copyright:

Journal keyword(s): protoplanetary disks - stars: pre-main sequence - planets and satellites: formation

Simbad objects: 51

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Number of rows : 51

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3602 3
2 V* FM Tau Or* 04 14 13.5839505100 +28 12 49.166941548 14.44   13.80 13.64   M0/2e 195 0
3 V* CW Tau Or* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 321 0
4 IRAS 04113+2758 ** 04 14 26.31 +28 06 04.5           ~ 58 0
5 V* FP Tau Or* 04 14 47.3027404423 +26 46 26.414740336 17.21 16.14 15.02     M4Ve 146 0
6 V* CX Tau Or* 04 14 47.8612023028 +26 48 11.013547235 16.48 15.93 14.50     M1.5Ve 157 0
7 V* CY Tau Or* 04 17 33.7281514373 +28 20 46.809969664 14.52 14.68 13.40 12.59   M1.5 240 0
8 V* DE Tau Or* 04 21 55.6346296353 +27 55 06.184221341 15.18 15.13 13.80     M3Ve 228 0
9 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 660 1
10 V* FT Tau Or* 04 23 39.1894939930 +24 56 14.248383831   16.15 14.93 14.70   M2.8 118 0
11 V* DH Tau Or* 04 29 41.5520056304 +26 32 58.123761109 15.14 14.62 13.10 13.01   M1Ve 271 0
12 V* IQ Tau Or* 04 29 51.5569553814 +26 06 44.854858369 15.43   13.80 12.28 11.11 M0.5 205 0
13 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1243 0
14 V* DK Tau A * 04 30 44.2409691803 +26 01 24.730398215           K5Ve 249 0
15 V* DK Tau Or* 04 30 44.243376 +26 01 24.65328 13.32 14.59 13.05 12.08   K7e+K7e 302 0
16 EM* LkHA 358 TT* 04 31 36.1396524070 +18 13 43.176961457     19.0     M0.9 89 0
17 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1237 0
18 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
19 V* GG Tau Or* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 662 1
20 V* FY Tau Or* 04 32 30.5786392247 +24 19 57.364725369 17.83 18.05 13.49 14.17   M0.1 101 0
21 V* FZ Tau Or* 04 32 31.7629319321 +24 20 03.057541003 16.15     15.04   M0 123 0
22 V* UZ Tau B TT* 04 32 42.82968 +25 52 31.4148   14.07 12.72 13.35   M1/3Ve 140 0
23 IRAS S04301+2608 Y*O 04 33 14.3602980976 +26 14 23.494786529           M0 34 0
24 V* GK Tau Or* 04 33 34.5626781676 +24 21 05.854541262 15.50   13.00 12.02 10.62 K7:Ve 280 0
25 V* DL Tau Or* 04 33 39.0766866461 +25 20 38.097973550 14.04 14.59 13.40 11.85 10.89 K7Ve 292 0
26 V* DM Tau Or* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 529 0
27 V* CI Tau Or* 04 33 52.0144455735 +22 50 30.093741884 14.97 15.09 13.80     K4IVe 282 1
28 V* AA Tau Or* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 644 0
29 V* HO Tau Or* 04 35 20.2103777721 +22 32 14.557063236     15.20     M0.5 110 0
30 V* DN Tau Or* 04 35 27.3776240781 +24 14 58.908761629 13.56 12.88 11.50 11.79   M1:Ve 355 0
31 Haro 6-28 Or* 04 35 56.8652987075 +22 54 35.826437972 18.94         M3.1 86 0
32 V* DO Tau Or* 04 38 28.5882167490 +26 10 49.472067634 12.78 13.44 12.30 13.01   M1Ve 325 1
33 IRAS 0437+257P08 TT? 04 39 55.7451364657 +25 45 01.943057594           B5 161 1
34 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3615 0
35 V* DP Tau Or* 04 42 37.6996387891 +25 15 36.992730557 15.84 15.2 13.70 14.42   M0.8 155 1
36 V* GO Tau Or* 04 43 03.0761884276 +25 20 18.708294279   16.2 14.40     M2.3 159 0
37 V* DR Tau Or* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 482 0
38 V* DS Tau Or* 04 47 48.5954846337 +29 25 11.189809829 13.11 13.16 12.30 12.37 10.80 K4Ve 217 0
39 V* UY Aur Or* 04 51 47.3900418279 +30 47 13.552212742 12.82 12.96 11.90 10.59 9.52 M0e+M2.5e 332 0
40 Haro 6-39 Y*O 04 52 09.6980531109 +30 37 45.414446427           M 27 0
41 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 565 0
42 V* SU Aur Or* 04 55 59.3861369488 +30 34 01.499800471   10.33 9.30 9.17   G2IIIne 544 0
43 QSO J0530+13 QSO 05 30 56.41672 +13 31 55.1495     20.0 19.35   ~ 889 1
44 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2031 1
45 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 264 0
46 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1587 1
47 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 704 0
48 NAME Lup Cloud SFR 16 03 -38.1           ~ 545 0
49 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3114 1
50 HD 150193 Be* 16 40 17.9242900066 -23 53 45.192676418 9.69 9.32 8.79 8.41   B9.5Ve 296 0
51 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 714 0

    Equat.    Gal    SGal    Ecl

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2021.01.26-01:38:50

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