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


Query : 2010A&A...512A..15R

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 - 2023
#notes
1 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 3859 3
2 V* FM Tau Or* 04 14 13.5841955640 +28 12 49.168982592 14.44   13.80 13.64   M0/2e 208 0
3 V* CW Tau TT* 04 14 17.0042670144 +28 10 57.766508508 13.92 13.64 12.36 12.86   K0Ve 344 0
4 IRAS 04113+2758 ** 04 14 26.31 +28 06 04.5           ~ 60 0
5 V* FP Tau Or* 04 14 47.3033083488 +26 46 26.414391720 17.21 16.14 15.02     M4Ve 160 0
6 V* CX Tau Or* 04 14 47.8615248984 +26 48 11.014877916 16.48 15.93 14.50     M1.5Ve 173 0
7 V* CY Tau Or* 04 17 33.7284990744 +28 20 46.812121656 14.52 14.68 13.40 12.59   M1.5 257 0
8 V* DE Tau Or* 04 21 55.6347850824 +27 55 06.184016436 15.18 15.13 13.80     M3Ve 246 0
9 V* RY Tau Or* 04 21 57.4092550080 +28 26 35.555316612 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 684 1
10 V* FT Tau Or* 04 23 39.1888788312 +24 56 14.250818940   16.15 14.93 14.70   M2.8 131 0
11 V* DH Tau Or* 04 29 41.5525353432 +26 32 58.126559604 15.14 14.62 13.10 13.01   M1Ve 289 0
12 V* IQ Tau Or* 04 29 51.5569574040 +26 06 44.859710736 15.43   13.80 12.28 11.11 M0.5 226 0
13 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1318 0
14 V* DK Tau A * 04 30 44.2408811328 +26 01 24.734232948           K5Ve 256 0
15 V* DK Tau Or* 04 30 44.243376 +26 01 24.65328 13.32 14.59 13.05 12.08   K7e+K7e 318 0
16 EM* LkHA 358 TT* 04 31 36.1433863008 +18 13 43.204853460     19.0     M0.9 92 0
17 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1360 0
18 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
19 V* GG Tau Or* 04 32 30.3506925552 +17 31 40.494063144 14.84 14.78 13.40 11.54   M0e+M2.0e 709 1
20 V* FY Tau Or* 04 32 30.5784243120 +24 19 57.359889192 17.83 18.05 13.49 14.17   M0.1 111 0
21 V* FZ Tau Or* 04 32 31.7627107344 +24 20 03.056011548 16.15     15.04   M0 135 0
22 V* UZ Tau B TT* 04 32 42.8118779016 +25 52 31.198173600   14.07 12.72 13.35   M1/3Ve 145 0
23 IRAS S04301+2608 Y*O 04 33 14.3617327872 +26 14 23.463738708           M0 40 1
24 V* GK Tau Or* 04 33 34.5630097872 +24 21 05.855136732 15.50   13.00 12.02 10.62 K7:Ve 294 0
25 V* DL Tau Or* 04 33 39.0767679288 +25 20 38.101382952 14.04 14.59 13.40 11.85 10.89 K7Ve 319 0
26 V* DM Tau Or* 04 33 48.7336763736 +18 10 09.973460280 14.30 14.82 14.00     M2Ve 596 0
27 V* CI Tau Or* 04 33 52.0143963264 +22 50 30.094090908 14.97 15.09 13.80     K4IVe 323 1
28 V* AA Tau Or* 04 34 55.4201902392 +24 28 53.033624580 13.14 13.34 12.20 12.03   K5Ve 699 0
29 V* HO Tau Or* 04 35 20.2104968376 +22 32 14.561379276     15.20     M0.5 124 0
30 V* DN Tau Or* 04 35 27.3776226144 +24 14 58.910343720 13.56 12.88 11.50 11.79   M1:Ve 374 0
31 Haro 6-28 Or* 04 35 56.8536876816 +22 54 36.092202012 18.94         M3.1 97 0
32 V* DO Tau Or* 04 38 28.5880527336 +26 10 49.467596196 12.78 13.44 12.30 13.01   M1Ve 348 1
33 IRAS 0437+257P08 Y*O 04 39 55.7457478224 +25 45 01.941104988           B5 168 1
34 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4099 0
35 V* DP Tau Or* 04 42 37.6989071232 +25 15 36.983641716 15.84 15.2 13.70 14.42   M0.8 166 1
36 V* GO Tau Or* 04 43 03.0761840904 +25 20 18.706850340   16.2 14.40     M2.3 183 0
37 V* DR Tau Or* 04 47 06.2151561264 +16 58 42.813872580 12.03 11.86 10.50 12.19   K5Ve 511 0
38 V* DS Tau Or* 04 47 48.5954691000 +29 25 11.191621512 13.11 13.16 12.30 12.37 10.80 K4Ve 238 0
39 V* UY Aur Or* 04 51 47.3890167432 +30 47 13.551561492 12.82 12.96 11.90 10.59 9.52 M0e+M2.5e 347 0
40 Haro 6-39 Y*O 04 52 09.7010929560 +30 37 45.414159924           M 29 0
41 V* GM Aur Or* 04 55 10.9815576936 +30 21 59.373771876 14.59 13.351 12.242 11.798   K3Ve 638 0
42 V* SU Aur Or* 04 55 59.3866872552 +30 34 01.499608092   10.33 9.30 9.17   G2IIIne 574 0
43 QSO J0530+13 Bla 05 30 56.41674741 +13 31 55.1494688     20.0 19.35   ~ 926 1
44 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2209 1
45 V* CQ Tau Ae* 05 35 58.4666264136 +24 44 54.091450572 11.290 10.780 10.000   8.33 F5IVe 287 0
46 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1791 1
47 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 760 0
48 NAME Lupus Complex SFR 16 03 -38.1           ~ 643 0
49 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3448 1
50 HD 150193 Be* 16 40 17.9243127240 -23 53 45.193372692 9.69 9.32 8.79 8.41   B9.5Ve 307 0
51 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 772 0

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2023.02.04-11:05:16

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