2017A&A...597A..72A


C.D.S. - SIMBAD4 rel 1.7 - 2020.06.06CEST04:37:14

2017A&A...597A..72A - Astronomy and Astrophysics, volume 597A, 72-72 (2017/1-1)

Mid-IR water and silicate relation in protoplanetary disks.

ANTONELLINI S., BREMER J., KAMP I., RIVIERE-MARICHALAR P., LAHUIS F., THI W.-F., WOITKE P., MEIJERINK R., ARESU G. and SPAANS M.

Abstract (from CDS):

Context. Mid-IR water lines from protoplanetary disks around T Tauri stars have a detection rate of 50%. Models have identified multiple physical properties of disks such as dust-to-gas mass ratio, dust size power law distribution, disk gas mass, disk inner radius, and disk scale height as potential explanations for the current detection rate.
Aims. In this study, we aim to break degeneracies through constraints obtained from observations. We search for a connection between mid-IR water line fluxes and the strength of the 10µm silicate feature.
Methods. We analyze observed water line fluxes from three blends at 15.17, 17.22 and 29.85µm published earlier and compute the 10µm silicate feature strength from Spitzer spectra to search for possible trends. We use a series of published ProDiMo thermo-chemical models, to explore disk dust and gas properties, and also the effects of different central stars. In addition, we produced two standard models with different dust opacity functions, and one with a parametric prescription for the dust settling.
Results. Our series of models that vary properties of the grain size distribution suggest that mid-IR water emission anticorrelates with the strength of the 10µm silicate feature. The models also show that the increasing stellar bolometric luminosity simultaneously enhance the strength of this dust feature and the water lines fluxes. No correlation is found between the observed mid-IR water lines and the 10µm silicate strength. Two-thirds of the targets in our sample show crystalline dust features, and the disks are mainly flaring. Our sample shows the same difference in the peak strength between amorphous and crystalline silicates that was noted in earlier studies, but our models do not support this intrinsic difference in silicate peak strength. Individual properties of our models are not able to reproduce the most extreme observations, suggesting that more complex dust properties (e.g., vertically changing) are required to reproduce the strongest 10µm silicate features. A parametrized settling prescription is able to boost the peak strength by a factor of 2 for the standard model. Water line fluxes are unrelated to the composition of the dust. The pronounced regular trends seen in the model results are washed out in the data due to the larger diversity in stellar and disk properties compared to our series of model.
Conclusions. The independent nature of the water line emission and the 10µm silicate strength found in observations, and the modeling results, leave as a possible explanation that the disks with weaker mid-IR water line fluxes are depleted in gas or enhanced in dust in the inner 10au. In the case of gas depleted disks, settling produces very strong 10µm silicate features with strong peak strength. Observations of larger unbiased samples with JWST/MIRI and ALMA are essential to verify this hypothesis.

Abstract Copyright: © ESO 2017

Journal keyword(s): protoplanetary disks - line: formation - stars: pre-main sequence - circumstellar matter

Status at CDS:  

Simbad objects: 37

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Number of rows : 37

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 EM* LkHA 270 TT* 03 29 17.6756898303 +31 22 44.898266275   14.5       K2/3IIIe 75 0
2 EM* LkHA 271 Em* 03 29 21.8748368520 +31 15 36.245029969   14.0 14.3     K4.0 57 0
3 EM* LkHA 326 Em* 03 30 44.0132509711 +30 32 46.808287930     16     G 33 0
4 EM* LkHA 327 Em* 03 33 30.416 +31 10 50.41     15     K2 56 0
5 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 229 0
6 EM* LkHA 330 TT* 03 45 48.2804487421 +32 24 11.851014679   12.30 10.97     F7 120 0
7 V* IP Tau Or* 04 24 57.0823478325 +27 11 56.543062579   14.50   12.46   M0:Ve 190 0
8 V* V710 Tau ** 04 31 57.79848 +18 21 36.9396           ~ 152 0
9 V* V710 Tau A TT* 04 31 57.8032267772 +18 21 34.726898440       13.87   M2/3e 152 0
10 V* AA Tau Or* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 622 0
11 CoKu Tau-Aur Star 4 TT* 04 41 16.8106225314 +28 40 00.077173462   16.40 14.68 14.59   M1.5e 165 0
12 V* DR Tau Or* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 466 0
13 V* SX Cha Or* 10 55 59.802000 -77 24 40.12524   16.01 14.57 14.23 12.35 M1.5+M3 79 0
14 V* SY Cha Or* 10 56 30.3882538728 -77 11 39.402450501         11.29 K5Ve 112 0
15 V* TW Cha Or* 10 59 01.0608276980 -77 22 40.946475900     13.40   11.68 K8Ve 114 0
16 V* VW Cha Or* 11 08 01.3974165580 -77 42 28.579297348 13.91 14.04 12.80   10.69 K7+M0 166 0
17 V* VZ Cha Or* 11 09 23.7736314968 -76 23 20.855918834   13.82 12.94   12.14 K7e 122 0
18 V* WX Cha Or* 11 09 58.666944 -77 37 09.03432   14.93 13.85 14.23 12.20 M1+M5 89 0
19 V* XX Cha Or* 11 11 39.6733333784 -76 20 15.037536625   16.67 15.28   12.56 M3Ve 96 1
20 NAME Cha Dark Cloud SFR 11 55 -78.0           ~ 554 1
21 Sz 50 Y*O 13 00 55.3820751133 -77 10 22.247668674   17.64 16.01     M3 41 0
22 V* GU Lup RR* 15 28 23.6427305880 -30 54 44.341358376     15.40     ~ 5 0
23 CD-33 10685 Or* 15 45 12.8670160092 -34 17 30.646921079 12.47 11.56 10.224 9.60 8.685 K3Ve 216 1
24 CD-35 10525 Or* 15 49 12.1055573607 -35 39 05.053991067 12.19 12.76 11.66 11.15   K7Ve 236 0
25 THA 15-12 Or* 15 56 09.2067120748 -37 56 06.126159332   13.12 11.93 11.45   M0e 242 0
26 V* RU Lup Or* 15 56 42.3109948086 -37 49 15.473469159 9.27 10.07 9.60     K7/M0e 378 0
27 V* RY Lup Or* 15 59 28.3852522995 -40 21 51.255321659   12.62 9.90     G8/K1IV-V 165 0
28 NAME Lup Cloud SFR 16 03 -38.1           ~ 514 0
29 HD 325367 Or* 16 03 05.4914377137 -40 18 25.426543472   11.40 8.50     M0 274 0
30 V* V866 Sco Or* 16 11 31.345632 -18 38 25.96200   13.98 12.63 12.81   K0e+K5e 243 0
31 Haro 1-1 Or* 16 21 34.7046243951 -26 12 26.914958774   14.59       K5e 56 0
32 Haro 1-4 Or* 16 25 10.508136 -23 19 14.78820       13.15   K4e 70 0
33 Haro 1-16 Or* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 174 0
34 Haro 1-17 Y*O 16 32 21.9312543188 -24 42 14.835977855   16.76 15.61     M2.5e 35 0
35 V* V1003 Oph Or* 16 34 09.1694383329 -15 48 16.776308800           G5 87 0
36 Hen 3-1258 Or* 16 48 45.6323559591 -14 16 35.849943900   14.94 13.34 12.84   K6 81 0
37 EM* AS 209 Or* 16 49 15.3035547820 -14 22 08.642015783   12.62 11.28     K4Ve 227 0

    Equat.    Gal    SGal    Ecl

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2020.06.06-04:37:14

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