2012ApJ...752...75C


Query : 2012ApJ...752...75C

2012ApJ...752...75C - Astrophys. J., 752, 75 (2012/June-2)

Submillimeter array observations of the RX J1633.9-2442 transition disk: evidence for multiple planets in the making.

CIEZA L.A., MATHEWS G.S., WILLIAMS J.P., MENARD F.C., KRAUS A.L., SCHREIBER M.R., ROMERO G.A., ORELLANA M. and IRELAND M.J.

Abstract (from CDS):

We present continuum high-resolution Submillimeter Array (SMA) observations of the transition disk object RX J1633.9-2442, which is located in the Ophiuchus molecular cloud and has recently been identified as a likely site of ongoing giant planet formation. The observations were taken at 340 GHz (880 µm) with the SMA in its most extended configuration, resulting in an angular resolution of 0".3 (35 AU at the distance of the target). We find that the disk is highly inclined (i ∼ 50°) and has an inner cavity ∼25 AU in radius, which is clearly resolved by our observations. We simultaneously model the entire optical to millimeter wavelength spectral energy distribution and SMA visibilities of RX J1633.9-2442 in order to constrain the structure of its disk. We find that an empty cavity ∼25 AU in radius is inconsistent with the excess emission observed at 12, 22, and 24 µm. Instead, the mid-IR excess can be modeled by either a narrow, optically thick ring at ∼10 AU or an optically thin region extending from ∼7 AU to ∼25 AU. The inner disk (r ≲ 5 AU) is mostly depleted of small dust grains as attested by the lack of detectable near-IR excess. We also present deep Keck aperture masking observations in the near-IR, which rule out the presence of a companion up to 500 times fainter than the primary star (in K band) for projected separations in the 5-20 AU range. We argue that the complex structure of the RX J1633.9-2442 disk is best explained by multiple planets embedded within the disk. We also suggest that the properties and incidence of objects such as RX J1633.9-2442, T Cha, and LkCa 15 (and those of the companions recently identified to these two latter objects) are most consistent with the runaway gas accretion phase of the core accretion model, when giant planets gain their envelopes and suddenly become massive enough to open wide gaps in the disk.

Abstract Copyright:

Journal keyword(s): circumstellar matter - protoplanetary disks - stars: individual: RX J1633.9-2442 - submillimeter: planetary systems

Simbad objects: 12

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Number of rows : 12
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 670 1
2 V* UX Tau A TT* 04 30 03.9931880444 +18 13 49.476948664   12.92 11.15     K2Ve 336 0
3 V* UX Tau Or* 04 30 03.99626 +18 13 49.4355 11.23 11.84 10.80 9.83 9.05 K2Ve+M1Ve 326 0
4 V* DM Tau Or* 04 33 48.7335659850 +18 10 09.974471722 14.30 14.82 14.00     M2Ve 557 0
5 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 595 1
6 CoKu Tau-Aur Star 4 TT* 04 41 16.8106225314 +28 40 00.077173462   16.40 14.68 14.59   M1.5e 171 0
7 V* GM Aur Or* 04 55 10.9813656049 +30 21 59.375978047 14.59 13.351 12.242 11.798   K3Ve 578 0
8 V* T Cha Or* 11 57 13.5268556629 -79 21 31.521755129   10.00 11.86     K0e 249 1
9 RX J1604.3-2130 X 16 04.3 -21 30           ~ 28 0
10 WRAY 15-1443 TT* 16 15 20.2339854383 -32 55 05.097043020 13.88 13.22 12.00 11.21 10.50 K5 74 0
11 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3246 1
12 2MASS J16335560-2442049 Y*O 16 33 55.6149601032 -24 42 05.006785530           K7 44 0

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2021.12.06-20:04:26

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