2010ApJ...717..441E


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.18CEST10:33:59

2010ApJ...717..441E - Astrophys. J., 717, 441-457 (2010/July-1)

Unveiling the structure of pre-transitional disks.

ESPAILLAT C., D'ALESSIO P., HERNANDEZ J., NAGEL E., LUHMAN K.L., WATSON D.M., CALVET N., MUZEROLLE J. and McCLURE M.

Abstract (from CDS):

In the past few years, several disks with inner holes that are relatively empty of small dust grains have been detected and are known as transitional disks. Recently, Spitzer has identified a new class of "pre-transitional disks" with gaps based on near-infrared photometry and mid-infrared spectra; these objects have an optically thick inner disk separated from an optically thick outer disk by an optically thin disk gap. A near-infrared spectrum provided the first confirmation of a gap in the pre-transitional disk of LkCa 15 by verifying that the near-infrared excess emission in this object was due to an optically thick inner disk. Here, we investigate the difference between the nature of the inner regions of transitional and pre-transitional disks using the same veiling-based technique to extract the near-infrared excess emission above the stellar photosphere. However, in this work we use detailed disk models to fit the excess continua as opposed to the simple blackbody fits previously used. We show that the near-infrared excess emission of the previously identified pre-transitional disks of LkCa 15 and UX Tau A in the Taurus cloud as well as the newly identified pre-transitional disk of ROX 44 in Ophiuchus can be fit with an inner disk wall located at the dust destruction radius. We also present detailed modeling of the broadband spectral energy distributions of these objects, taking into account the effect of shadowing by the inner disk on the outer disk, but considering the finite size of the star, unlike other recent treatments. The near-infrared excess continua of these three pre-transitional disks, which can be explained by optically thick inner disks, are significantly different from that of the transitional disks of GM Aur, whose near-infrared excess continuum can be reproduced by emission from sub-micron-sized optically thin dust, and DM Tau, whose near-infrared spectrum is consistent with a disk hole that is relatively free of small dust. The structure of pre-transitional disks may be a sign of young planets forming in these disks and future studies of pre-transitional disks will provide constraints to aid in theoretical modeling of planet formation.

Abstract Copyright:

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

Simbad objects: 22

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Number of rows : 22

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 HD 25175 * 04 00 36.8877857685 +17 17 47.971091271   6.352 6.305     A0V 46 0
2 HD 27761 * 04 23 26.9731791527 +16 37 45.857393734   8.43 8.13     A0V 16 0
3 * 55 Per * 04 24 29.1555998134 +34 07 50.735409994   5.657 5.718     B8V 53 0
4 V* UX Tau A TT* 04 30 03.9931880444 +18 13 49.476948664   12.92 11.15     K2Ve 333 0
5 V* UX Tau Or* 04 30 03.99626 +18 13 49.4355 11.23 11.84 10.80 9.83 9.05 K2Ve+M1Ve 319 0
6 V* DM Tau Or* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 538 0
7 V* V1115 Tau TT* 04 36 19.1014976181 +25 42 58.999936422   12.97 11.76 10.81 10.228 M0 80 0
8 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 581 1
9 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3680 0
10 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 567 0
11 CVSO 224 TT* 05 25 46.7558569125 +01 43 30.293019729     17.21 16.19 14.61 M3.5Ve 24 0
12 HD 36003 PM* 05 28 26.0954741443 -03 29 58.396897793 9.864 8.777 7.642 6.968 6.401 K5V 188 0
13 HD 42581 Er* 06 10 34.6152510171 -21 51 52.658021185 10.801 9.607 8.125 7.164 6.121 M1V 414 0
14 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1612 1
15 V* CS Cha Or* 11 02 24.8849252208 -77 33 35.683462615   12.88 11.69   10.123 K2Ve 201 0
16 Ass Cha T 2-54 TT* 11 12 42.6696152636 -77 22 22.928829312     11.103   9.653 G8+K7 80 2
17 * 61 UMa PM* 11 41 03.0159358291 +34 12 05.882438337 6.31 6.08 5.34 4.73 4.38 G8V 576 0
18 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 712 0
19 HD 146606 * 16 18 16.1596445036 -28 02 30.144571751   7.05 7.06     A0V 57 0
20 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3156 1
21 Haro 1-16 Or* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 187 0
22 HD 219134 Er* 23 13 16.9747821012 +57 10 06.076520993 7.460 6.560 5.570 4.76 4.23 K3V 533 1

    Equat.    Gal    SGal    Ecl

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2021.04.18-10:33:59

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