2018A&A...610A..24F


Query : 2018A&A...610A..24F

2018A&A...610A..24F - Astronomy and Astrophysics, volume 610A, 24-24 (2018/2-1)

ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet.

FEDELE D., TAZZARI M., BOOTH R., TESTI L., CLARKE C.J., PASCUCCI I., KOSPAL A., SEMENOV D., BRUDERER S., HENNING T. and TEAGUE R.

Abstract (from CDS):

This paper presents new high angular resolution ALMA 1.3mm dust continuum observations of the protoplanetary system AS 209 in the Ophiuchus star forming region. The dust continuum emission is characterized by a main central core and two prominent rings at r=75au and r=130au intervaled by two gaps at r=62au and r=103au. The two gaps have different widths and depths, with the inner one being narrower and shallower. We determined the surface density of the millimeter dust grains using the 3D radiative transfer disk code DALI. According to our fiducial model the inner gap is partially filled with millimeter grains while the outer gap is largely devoid of dust. The inferred surface density is compared to 3D hydrodynamical simulations (FARGO-3D) of planet-disk interaction. The outer dust gap is consistent with the presence of a giant planet (Mplanet∼0.7MSaturn); the planet is responsible for the gap opening and for the pile-up of dust at the outer edge of the planet orbit. The simulations also show that the same planet could be the origin of the inner gap at r=62au. The relative position of the two dust gaps is close to the 2:1 resonance and we have investigated the possibility of a second planet inside the inner gap. The resulting surface density (including location, width and depth of the two dust gaps) are in agreement with the observations. The properties of the inner gap pose a strong constraint to the mass of the inner planet (Mplanet<0.1MJ). In both scenarios (single or pair of planets), the hydrodynamical simulations suggest a very low disk viscosity (α<10–4). Given the young age of the system (0.5-1Myr), this result implies that the formation of giant planets occurs on a timescale of ≤1Myr.

Abstract Copyright: © ESO, 2018

Journal keyword(s): protoplanetary disks - planet-disk interactions

VizieR on-line data: <Available at CDS (J/A+A/610/A24): list.dat fits/*>

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 - 2022
#notes
1 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1319 0
2 V* AA Tau Or* 04 34 55.4201902392 +24 28 53.033624580 13.14 13.34 12.20     K5Ve 679 0
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 B1514-24 BLL 15 17 41.8134049824 -24 22 19.482207024   15.13 14.00 13.95   ~ 697 3
5 EM* AS 209 Or* 16 49 15.3034917000 -14 22 08.643317664   12.62 11.28     K4Ve 303 0
6 QSO B1730-130 QSO 17 33 02.7055087032 -13 04 49.545516612   18 18.5 18.78 17.39 ~ 1058 1
7 HD 163296 Ae* 17 56 21.2881851168 -21 57 21.871819008 7.00 6.93 6.85 6.86 6.67 A1Vep 953 0
8 HD 169142 Ae* 18 24 29.7799891464 -29 46 49.327400568   8.42 8.16     F1VekA3mA3_lB? 387 2

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2022.05.28-10:46:03

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