2016A&A...585A..58V


Query : 2016A&A...585A..58V

2016A&A...585A..58V - Astronomy and Astrophysics, volume 585A, 58-58 (2016/1-1)

Resolved gas cavities in transitional disks inferred from CO isotopologs with ALMA.

VAN DER MAREL N., VAN DISHOECK E.F., BRUDERER S., ANDREWS S.M., PONTOPPIDAN K.M., HERCZEG G.J., VAN KEMPEN T. and MIOTELLO A.

Abstract (from CDS):

Transitional disks around young stars with large dust cavities are promising candidates to look for recently formed, embedded planets. Models of planet-disk interaction predict that young planets clear a gap in the gas while trapping dust at larger radii. Other physical mechanisms might also be responsible for cavities. Previous observations have revealed that gas is still present inside these cavities, but the spatial distribution of this gas remains uncertain. We present high spatial resolution observations with the Atacama Large Millimeter/submillimeter Array (ALMA) of 13CO and C18O 3-2 or 6-5 lines of four well-studied transitional disks around pre-main-sequence stars with large dust cavities. The line and continuum observations are used to set constraints on the the gas surface density, specifically on the cavity size and density drop inside the cavity. The physical-chemical model DALI was used to analyze the gas images of SR21, HD 135344B (also known as SAO 206462), DoAr44, and IRS 48. The main parameters of interest are the size, depth and shape of the gas cavity in each of the disks. CO isotope-selective photodissociation is included to properly constrain the surface density in the outer disk from C18O emission. The gas cavities are up to three times smaller than those of the dust in all four disks. Model fits indicate that the surface density inside the gas cavities decreases by a factor of 100 to 10000 compared with the surface density profile derived from the outer disk. The data can be fit by either introducing one or two drops in the gas surface density or a surface density profile that increases with radius inside the cavity. A comparison with an analytical model of gap depths by planet-disk interaction shows that the disk viscosities are most likely low, between between 10–3 and 10–4, for reasonable estimates of planet masses of up to 10 Jupiter masses. The resolved measurements of the gas and dust in transition disk cavities support the predictions of models that describe how planet-disk interactions sculpt gas disk structures and influence the evolution of dust grains. These observed structures strongly suggest the presence of giant planetary companions in transition disk cavities, although at smaller orbital radii than is typically indicated from the dust cavity radii alone.

Abstract Copyright:

Journal keyword(s): astrochemistry - stars: formation - protoplanetary disks - ISM: molecules

Simbad objects: 16

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Number of rows : 16
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* GM Aur Or* 04 55 10.9815576936 +30 21 59.373771876 14.59 13.351 12.242 11.798   K3Ve 616 0
2 V* AB Aur Ae* 04 55 45.8458932216 +30 33 04.292077032 7.20 7.16 7.05 6.96 6.70 A0Ve 992 2
3 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1736 1
4 QSO B1424-41 QSO 14 27 56.2977548952 -42 06 19.437654096   18.48 17.7 16.30   ~ 423 1
5 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 410 1
6 QSO B1514-24 BLL 15 17 41.8134049824 -24 22 19.482207024   15.13 14.00 13.95   ~ 697 3
7 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 560 1
8 2MASS J16042165-2130284 Y*O 16 04 21.6547947840 -21 30 28.550063304   13.3       K2 106 0
9 QSO B1622-253 QSO 16 25 46.8886080600 -25 27 38.336613804   21.3 20.6 19.60   ~ 322 1
10 QSO B1622-297 Bla 16 26 06.0209027208 -29 51 26.968763916   18.41 20.5 17.6   ~ 387 0
11 EM* SR 21A TT* 16 27 10.2778380120 -24 19 12.622467720   16.08 14.10     G1 256 1
12 IRAS 16245-2423 TT* 16 27 37.1906433768 -24 30 35.025246828       16.66 14.67 B5-F2 263 0
13 Haro 1-16 Or* 16 31 33.4634997336 -24 27 37.158728076   14.02 12.80     K3e 205 0
14 DoAr 54 Em* 16 32.4 -24 06           ~ 2 0
15 QSO J1700-2610 QSO 17 00 53.1542036424 -26 10 51.722383908   16.50       ~ 97 1
16 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 953 0

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2022.05.25-09:54:37

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