2017A&A...598A.118C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST05:49:59

2017A&A...598A.118C - Astronomy and Astrophysics, volume 598A, 118-118 (2017/2-1)

A gas density drop in the inner 6 AU of the transition disk around the Herbig Ae star HD 139614. Further evidence for a giant planet inside the disk?

CARMONA A., THI W.F., KAMP I., BARUTEAU C., MATTER A., VAN DEN ANCKER M., PINTE C., KOSPAL A., AUDARD M., LIEBHART A., SICILIA-AGUILAR A., PINILLA P., REGALY Z., GUDEL M., HENNING T., CIEZA L.A., BALDOVIN-SAAVEDRA C., MEEUS G. and EIROA C.

Abstract (from CDS):

Context. Quantifying the gas surface density inside the dust cavities and gaps of transition disks is important to establish their origin.
Aims. We seek to constrain the surface density of warm gas in the inner disk of HD 139614, an accreting 9Myr Herbig Ae star with a (pre-)transition disk exhibiting a dust gap from 2.3±0.1 to 5.3±0.3AU.
Methods. We observed HD 139614 with ESO/VLT CRIRES and obtained high-resolution (R∼90000) spectra of CO ro-vibrational emission at 4.7µm. We derived constraints on the disk's structure by modeling the CO isotopolog line-profiles, the spectroastrometric signal, and the rotational diagrams using grids of flat Keplerian disk models.
Results. We detected υ = 1-0 12CO, 2-1 12CO, 1-0 13CO, 1-0 C18O, and 1-0 C17O ro-vibrational lines. Lines are consistent with disk emission and thermal excitation. 12CO υ=1-0 lines have an average width of 14km/s, Tgas of 450K and an emitting region from 1 to 15AU. 13CO and C18O lines are on average 70 and 100K colder, 1 and 4km/s narrower than 12CO υ=1-0, and are dominated by emission at R≥6AU. The 12CO υ=1-0 composite line-profile indicates that if there is a gap devoid of gas it must have a width narrower than 2AU. We find that a drop in the gas surface density (δgas) at R<5-6AU is required to be able to simultaneously reproduce the line-profiles and rotational diagrams of the three CO isotopologs. Models without a gas density drop generate 13CO and C18O emission lines that are too broad and warm. The value of δgas can range from 10–2 to 10–4 depending on the gas-to-dust ratio of the outer disk. We find that the gas surface density profile at 1<R<6AU is flat or increases with radius. We derive a gas column density at 1<R<6AU of NH=3x1019-1021cm–2 (7x10–5-2.4x10–3g/cm2) assuming NCO=10–4NH. We find a 5σ upper limit on the CO column density NCO at R≤1AU of 5x1015cm–2 (NH≤5x1019cm–2).
Conclusions. The dust gap in the disk of HD 139614 has molecular gas. The distribution and amount of gas at R≤6AU in HD 139614 is very different from that of a primordial disk. The gas surface density in the disk at R≤1AU and at 1<R<6AU is significantly lower than the surface density that would be expected from the accretion rate of HD 139614 (10–8M/yr) assuming a standard viscous α-disk model. The gas density drop, the non-negative density gradient in the gas inside 6AU, and the absence of a wide (>2AU) gas gap, suggest the presence of an embedded <2MJ planet at around 4AU.

Abstract Copyright: © ESO, 2017

Journal keyword(s): protoplanetary disks - stars: pre-main sequence - planets and satellites: formation - techniques: spectroscopic - stars: variables: T Tauri, Herbig Ae/Be

Simbad objects: 13

goto Full paper

goto View the reference in ADS

Number of rows : 13

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 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 552 1
2 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 651 1
3 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 357 1
4 HD 139614 pr* 15 40 46.3818973118 -42 29 53.538928508   8.47 8.24     A9VekA5mA5(_lB) 160 0
5 * g Lup PM* 15 41 11.3769921 -44 39 40.342813   5.04 4.64     F3/5V 178 0
6 Ass Sco OB 2-3 * 15 49.7 -26 59           ~ 15 0
7 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 467 1
8 2MASS J16042165-2130284 pr* 16 04 21.6546714640 -21 30 28.549578725   13.3       K2 91 0
9 WRAY 15-1443 TT* 16 15 20.2339854383 -32 55 05.097043020 13.88 13.22 12.00 11.21 10.50 K5 66 0
10 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 233 1
11 IRAS 16245-2423 TT* 16 27 37.1911764648 -24 30 35.031583716       16.66 14.67 B5-F2 235 0
12 Haro 1-16 Or* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 175 0
13 V* VV CrA Or* 19 03 06.7419790029 -37 12 49.683383133   16.45 14.67 14.12 11.62 K7 107 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2017A&A...598A.118C and select 'bookmark this link' or equivalent in the popup menu


2020.07.13-05:49:59

© Université de Strasbourg/CNRS

    • Contact