2012A&A...540A...6R


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.17CET20:18:10

2012A&A...540A...6R - Astronomy and Astrophysics, volume 540A, 6-6 (2012/4-1)

The effect of local optically thick regions in the long-wave emission of young circumstellar disks.

RICCI L., TROTTA F., TESTI L., NATTA A., ISELLA A. and WILNER D.J.

Abstract (from CDS):

Multi-wavelength observations of protoplanetary disks in the sub-millimeter continuum have measured spectral indices values which are significantly lower than what is found in the diffuse interstellar medium. Under the assumption that mm-wave emission of disks is mostly optically thin, these data have been generally interpreted as evidence for the presence of mm/cm-sized pebbles in the disk outer regions. In this work we investigate the effect of possible local optically thick regions on the mm-wave emission of protoplanetary disks without mm/cm-sized grains. A significant local increase of the optical depth in the disk can be caused by the concentration of solid particles, as predicted to result from a variety of proposed physical mechanisms. We calculate the filling factors and implied overdensities these optically thick regions would need to significantly affect the millimeter fluxes of disks, and we discuss their plausibility. We find that optically thick regions characterized by relatively small filling factors can reproduce the mm-data of young disks without requesting emission from mm/cm-sized pebbles. However, these optically thick regions require dust overdensities much larger than what predicted by any of the physical processes proposed in the literature to drive the concentration of solids. We find that only for the most massive disks it is possible and plausible to imagine that the presence of optically thick regions in the disk is responsible for the low measured values of the mm spectral index. For the majority of the disk population, optically thin emission from a population of large mm-sized grains remains the most plausible explanation. The results of this analysis further strengthen the scenario for which the measured low spectral indices of protoplanetary disks at mm wavelengths are due to the presence of large mm/cm-sized pebbles in the disk outer regions.

Abstract Copyright:

Journal keyword(s): protoplanetary disks

CDS comments: Table 6 object 136-1955 not in Simbad.

Simbad objects: 64

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Number of rows : 64

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 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3464 3
2 4C 32.14 QSO 03 36 30.10760600 +32 18 29.3422210     17.50 16.6   ~ 568 1
3 V* FM Tau TT* 04 14 13.5839505100 +28 12 49.166941548 14.44   13.80 13.64   M0/2e 186 0
4 V* FN Tau TT* 04 14 14.5943659839 +28 27 58.063377983     14.70 13.68   M5 139 0
5 V* CW Tau TT* 04 14 17.0041128798 +28 10 57.765657757 13.92 13.64 12.36 12.86   K0Ve 310 0
6 [BHS98] MHO 1 TT* 04 14 26.2709425846 +28 06 03.288644046           M2.5 34 1
7 IRAS 04113+2758 ** 04 14 26.31 +28 06 04.5           ~ 57 0
8 [BHS98] MHO 2 TT* 04 14 26.4022247808 +28 05 59.640852985           M2.5 39 1
9 V* CX Tau TT* 04 14 47.8612023028 +26 48 11.013547235 16.48 15.93 14.50     M1.5Ve 143 0
10 V* CY Tau TT* 04 17 33.7281514373 +28 20 46.809969664 14.52 14.68 13.40 12.59   M1.5 223 0
11 3C 111 Sy1 04 18 21.2773655604 +38 01 35.801523843   19.75 18.05     ~ 841 1
12 V* V892 Tau Ae* 04 18 40.6120892867 +28 19 15.641672501   16.6 14.69 14.35   A0Ve 256 1
13 V* BP Tau TT* 04 19 15.8342975037 +29 06 26.929456808   13.13 12.12 11.89   K5/7Ve 584 0
14 V* DE Tau TT* 04 21 55.6346296353 +27 55 06.184221341 15.18 15.13 13.80     M3Ve 216 0
15 V* RY Tau TT* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 634 1
16 V* IQ Tau TT* 04 29 51.5569553814 +26 06 44.854858369 15.43   13.80 12.28 11.11 M0.5 191 0
17 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1182 1
18 V* FZ Tau TT* 04 32 31.7629319321 +24 20 03.057541003 16.15     15.04   M0 114 0
19 NAME UZ Tau B TT* 04 32 42.830 +25 52 31.41   14.07 12.72 13.35   M1/3Ve 131 0
20 V* DL Tau TT* 04 33 39.0766866461 +25 20 38.097973550 14.04 14.59 13.40 11.85 10.89 K7Ve 273 0
21 V* DM Tau TT* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 489 0
22 V* CI Tau TT* 04 33 52.0144455735 +22 50 30.093741884 14.97 15.09 13.80     K4IVe 245 0
23 V* AA Tau TT* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 601 0
24 V* HO Tau TT* 04 35 20.2103777721 +22 32 14.557063236     15.20     M0.5 103 0
25 V* DN Tau TT* 04 35 27.3776240781 +24 14 58.908761629 13.56 12.88 11.50 11.79   M1:Ve 339 0
26 V* DO Tau TT* 04 38 28.5882167490 +26 10 49.472067634 12.78 13.44 12.30 13.01   M1Ve 303 1
27 IRAS 0437+257P08 TT? 04 39 55.7451364657 +25 45 01.943057594           B5 158 1
28 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3322 0
29 V* GO Tau TT* 04 43 03.0761884276 +25 20 18.708294279   16.2 14.40     M2.3 145 0
30 V* DQ Tau TT* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 280 0
31 V* DR Tau TT* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 462 0
32 V* DS Tau TT* 04 47 48.5954846337 +29 25 11.189809829 13.11 13.16 12.30 12.37 10.80 K4Ve 201 0
33 QSO B0446+113 BLL 04 49 07.67110088 +11 21 28.5964577     20 18.58   ~ 218 1
34 V* GM Aur TT* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 533 0
35 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 900 2
36 V* SU Aur TT* 04 55 59.3861369488 +30 34 01.499800471   10.33 9.30 9.17   G2IIIne 525 0
37 V* V836 Tau TT* 05 03 06.5988350466 +25 23 19.604482133   14.66       K7/M0Ve 200 0
38 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1907 1
39 [BOM2000] d121-192 Y*O 05 35 12.0906622890 -05 19 24.750318345   15.5 20.92   15.581 M6 29 1
40 [BOM2000] d132-183 Y*O 05 35 13.23 -05 18 32.7         20.098 ~ 10 0
41 V* V2252 Ori Or* 05 35 14.0508534214 -05 19 52.019951394 16.713 15.615 14.602   12.579 G 46 1
42 M 42 HII 05 35 17.3 -05 23 28           ~ 3658 0
43 V* V2323 Ori Or* 05 35 18.1040864996 -05 28 25.097438355   18.990 18.772 16.09 16.157 M1:e 31 1
44 V* V2377 Ori Or* 05 35 21.5757535214 -05 09 38.822354154   15.1     15.509 K5 37 0
45 HH 668 HH 05 35 25.30 -05 15 35.5           ~ 15 0
46 2MASS J05352804-0517202 pr* 05 35 28.0443411068 -05 17 20.212518257   18.551 17.312   13.830 M4 33 1
47 EM* SR 4 TT* 16 25 56.1659484606 -24 20 48.239269835     12.80 11.7 10.7 K0:Ve 143 1
48 GSS 26 Y*O 16 26 10.33152 -24 20 54.8232           M0 69 1
49 Elia 2-20 TT* 16 26 18.8782824640 -24 28 19.698059817           ~ 87 1
50 DoAr 25 TT* 16 26 23.6911216715 -24 43 13.886717283       12.65   K5 118 0
51 Elia 2-24 TT* 16 26 24.0896068058 -24 16 13.456681632   16.3 14.40 15.81 13.97 K6 112 1
52 GSS 39 Y*O 16 26 45.0321556934 -24 23 07.808781522           M0 127 1
53 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 223 1
54 WL 3 Y*O 16 27 19.21584 -24 28 43.8528           K7 60 0
55 YLW 16C Y*O 16 27 26.48952 -24 39 23.0760           M1 51 0
56 YLW 47 TT* 16 27 38.3220493264 -24 36 58.601739078       17.69 15.52 M0 83 0
57 DoAr 33 TT* 16 27 39.0127002068 -23 58 18.708241197   15.7   13.24 12.02 K4 44 0
58 ROX 27 TT* 16 27 39.4297106587 -24 39 15.527875310       15.76 14.03 M0+M4 86 0
59 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2938 0
60 YLW 58 TT* 16 28 16.5131631203 -24 36 58.057875801   18.5   16.55 14.46 M4 79 0
61 Haro 1-16 TT* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 165 0
62 V* V1003 Oph TT* 16 34 09.1694383329 -15 48 16.776308800           G5 85 0
63 Hen 3-1258 TT* 16 48 45.6323559591 -14 16 35.849943900   14.94 13.34 12.84   K6 76 0
64 EM* AS 209 TT* 16 49 15.3035547820 -14 22 08.642015783   12.62 11.28     K4Ve 207 0

    Equat.    Gal    SGal    Ecl

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2019.11.17-20:18:10

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