2011ApJ...732...42A


C.D.S. - SIMBAD4 rel 1.7 - 2019.12.12CET20:57:44

2011ApJ...732...42A - Astrophys. J., 732, 42 (2011/May-1)

Resolved images of large cavities in protoplanetary transition disks.

ANDREWS S.M., WILNER D.J., ESPAILLAT C., HUGHES A.M., DULLEMOND C.P., McCLURE M.K., QI C. and BROWN J.M.

Abstract (from CDS):

Circumstellar disks are thought to experience a rapid "transition" phase in their evolution that can have a considerable impact on the formation and early development of planetary systems. We present new and archival high angular resolution (0".3 ~ 40-75 AU) Submillimeter Array (SMA) observations of the 880 µm (340 GHz) dust continuum emission from 12 such transition disks in nearby star-forming regions. In each case, we directly resolve a dust-depleted disk cavity around the central star. Using two-dimensional Monte Carlo radiative transfer calculations, we interpret these dust disk structures in a homogeneous, parametric model framework by reproducing their SMA continuum visibilities and spectral energy distributions. The cavities in these disks are large (Rcav= 15-73 AU) and substantially depleted of small (~µm-sized) dust grains, although their mass contents are still uncertain. The structures of the remnant material at larger radii are comparable to normal disks. We demonstrate that these large cavities are relatively common among the millimeter-bright disk population, comprising at least 1 in 5 (20%) of the disks in the bright half (and ≥ 26% of the upper quartile) of the millimeter luminosity (disk mass) distribution. Utilizing these results, we assess some of the physical mechanisms proposed to account for transition disk structures. As has been shown before, photoevaporation models do not produce the large cavity sizes, accretion rates, and disk masses representative of this sample. A sufficient decrease of the dust optical depths in these cavities by particle growth would be difficult to achieve: substantial growth (to meter sizes or beyond) must occur in large (tens of AU) regions of low turbulence without also producing an abundance of small particles. Given those challenges, we suggest instead that the observations are most commensurate with dynamical clearing due to tidal interactions with low-mass companions-very young (∼1 Myr) brown dwarfs or giant planets on long-period orbits.

Abstract Copyright:

Journal keyword(s): circumstellar matter - planet-disk interactions - planets and satellites: formation - protoplanetary disks - submillimeter: planetary systems

Simbad objects: 42

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Number of rows : 42

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 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1011 0
2 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 223 0
3 EM* LkHA 330 TT* 03 45 48.2804487421 +32 24 11.851014679   12.30 10.97     F7 116 0
4 3C 111 Sy1 04 18 21.2773655604 +38 01 35.801523843   19.75 18.05     ~ 841 1
5 V* RY Tau TT* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 636 1
6 V* DG Tau TT* 04 27 04.6913654419 +26 06 16.041555299 13.57 13.97 10.50 12.28   K6Ve 904 1
7 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1184 1
8 V* UX Tau B TT* 04 30 03.5778750604 +18 13 49.477040697       13.33   M1Ve 59 0
9 V* UX Tau C TT* 04 30 03.9885439206 +18 13 46.786269979     18.0     M5 32 0
10 V* UX Tau A TT* 04 30 03.9931880444 +18 13 49.476948664   12.92 11.15     K2Ve 321 0
11 V* UX Tau TT* 04 30 03.99626 +18 13 49.4355 11.23 11.84 10.80 9.83 9.05 K2Ve+M1Ve 308 0
12 V* HL Tau TT* 04 31 38.437 +18 13 57.65   16.02 15.10 14.21   K5 1137 0
13 IRAS 04287+1807 mul 04 31 38.8 +18 13 57           ~ 796 0
14 V* GG Tau TT* 04 32 30.3318954228 +17 31 40.834888327 14.84 14.78 13.40 11.54   M0e+M2.0e 630 1
15 Mrk 1506 Sy1 04 33 11.0958197353 +05 21 15.617543663   15.72 15.05 10.08   ~ 1814 2
16 V* DM Tau TT* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 492 0
17 EM* LkCa 15 TT* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 528 1
18 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3336 0
19 V* DQ Tau TT* 04 46 53.0577037389 +17 00 00.135310040 14.56 13.67 12.00 13.21   M1Ve 281 0
20 V* GM Aur TT* 04 55 10.9813656049 +30 21 59.375978047 14.59 14.22 13.10     K3Ve 534 0
21 QSO B0507+179 QSO 05 10 02.36912982 +18 00 41.5816534   20.0 19.0 19.09   ~ 282 1
22 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 327 0
23 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1454 1
24 HD 98800 RS* 11 22 05.28975 -24 46 39.7571   10.27 8.912 9.257 7.386 K5V(e) 322 0
25 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5253 1
26 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 332 1
27 NAME Lup Cloud SFR 16 03 -38.1           ~ 485 0
28 ICRF J160431.0-444131 Bla 16 04 31.02069 -44 41 31.9742   20.75       ~ 55 0
29 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1081 1
30 WRAY 15-1443 TT* 16 15 20.2339854383 -32 55 05.097043020 13.88 13.22 12.00 11.21 10.50 K5 61 0
31 QSO B1622-253 QSO 16 25 46.89164010 -25 27 38.3267989   21.3 20.6 19.60   ~ 291 1
32 QSO B1622-297 QSO 16 26 06.02083867 -29 51 26.9710860   18.41 20.5 17.6   ~ 355 0
33 Haro 1-7 ** 16 26 58.53 -24 45 35.3           K2:e+M0.5e 94 0
34 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 225 1
35 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2945 0
36 YLW 58 TT* 16 28 16.5131631203 -24 36 58.057875801   18.5   16.55 14.46 M4 81 0
37 Haro 1-16 TT* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 166 0
38 2MASS J16335560-2442049 Y*O 16 33 55.6149601033 -24 42 05.006785530           K7 39 0
39 * tau Oph ** 18 03 04.91992 -08 10 49.2586   5.17 4.78     F3IV 90 0
40 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2448 2
41 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1101 3
42 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 864 1

    Equat.    Gal    SGal    Ecl

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2019.12.12-20:57:44

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