2018A&A...617A...1K


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:24:12

2018A&A...617A...1K - Astronomy and Astrophysics, volume 617A, 1-1 (2018/9-1)

Diagnostic value of far-IR water ice features in T Tauri disks.

KAMP I., SCHEEPSTRA A., MIN M., KLARMANN L. and RIVIERE-MARICHALAR P.

Abstract (from CDS):


Aims. This paper investigates how the far-IR water ice features can be used to infer properties of disks around T Tauri stars and the water ice thermal history. We explore the power of future observations with SOFIA/HIRMES and SPICA's proposed far-IR instrument SAFARI.
Methods. A series of detailed radiative transfer disk models around a representative T Tauri star are used to investigate how the far-IR water ice features at 45 and 63µm change with key disk properties: disk size, grain sizes, disk dust mass, dust settling, and ice thickness. In addition, a series of models is devised to calculate the water ice emission features from warmup, direct deposit, and cooldown scenarios of the water ice in disks.
Results. Photodesorption from icy grains in disk surfaces weakens the mid-IR water ice features by factors of 4-5. The far-IR water ice emission features originate from small grains at the surface snow line in disks at distance of 10-100 au. Unless this reservoir is missing in disks (e.g., transitional disks with large cavities), the feature strength does not change. Grains larger than 10µm do not contribute to the features. Grain settling (using turbulent description) affects the strength of the ice features by at most 15%. The strength of the ice feature scales with the disk dust mass and water ice fraction on the grains, but saturates for dust masses higher than 10–4M and for ice mantles that increase the dust mass by more than 50%. The various thermal histories of water ice leave an imprint on the shape of the features (crystalline and/or amorphous) and on the peak strength and position of the 45µm feature. SOFIA/HIRMES can only detect crystalline ice features that are much stronger than those simulated in our standard T Tauri disk model in deep exposures (1h). SPICA/SAFARI can detect the typical ice features in our standard T Tauri disk model in short exposures (10min).
Conclusions. The sensitivity of SPICA/SAFARI will allow the detailed study of the 45 and 63µm water ice feature in unbiased surveys of T Tauri stars in nearby star forming regions and an estimate of the mass of their ice reservoir. The water ice emission features carry an imprint of the thermal history of the ice, and thus can distinguish between various formation and transport scenarios. Amorphous ice at 45µm that has a much broader and flatter peak could be detected in deep surveys if the underlying continuum can be well characterized and the baseline stability of SAFARI is better than a few percent.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: low-mass - stars: pre-main sequence - infrared: planetary systems - protoplanetary disks

Simbad objects: 8

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Number of rows : 8

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* DG Tau Or* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 923 1
2 Haro 6-13 Or* 04 32 15.4177438039 +24 28 59.580866027 19.22   17.7     M0 181 1
3 V* AA Tau Or* 04 34 55.4222683130 +24 28 53.038273587 13.14 13.34 12.20     K5Ve 625 0
4 V* DO Tau Or* 04 38 28.5882167490 +26 10 49.472067634 12.78 13.44 12.30 13.01   M1Ve 313 1
5 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 255 0
6 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1532 1
7 CD-35 10525 Or* 15 49 12.1055573607 -35 39 05.053991067 12.19 12.76 11.66 11.15   K7Ve 237 0
8 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 467 1

    Equat.    Gal    SGal    Ecl

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2020.07.08-03:24:12

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