2009A&A...508..787K


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.28CET20:55:27

2009A&A...508..787K - Astronomy and Astrophysics, volume 508, 787-803 (2009/12-3)

Revealing the sub-AU asymmetries of the inner dust rim in the disk around the Herbig Ae star R Coronae Austrinae.

KRAUS S., HOFMANN K.-H., MALBET F., MEILLAND A., NATTA A., SCHERTL D., STEE P. and WEIGELT G.

Abstract (from CDS):

Unveiling the structure of the disks around intermediate-mass pre-main-sequence stars (Herbig Ae/Be stars) is essential for our understanding of the star and planet formation process. In particular, models predict that in the innermost AU around the star, the dust disk forms a ``puffed-up'' inner rim, which should result in a strongly asymmetric brightness distribution for disks seen under intermediate inclination. Our aim is to constrain the sub-AU geometry of the inner disk around the Herbig Ae star R CrA and search for the predicted asymmetries. Using the VLTI/AMBER long-baseline interferometer, we obtained 24 near-infrared (H- and K-band) spectro-interferometric observations on R CrA. Observing with three telescopes in a linear array configuration, each data set samples three equally spaced points in the visibility function, providing direct information about the radial intensity profile. In addition, the observations cover a wide position angle range (∼97°), also probing the position angle dependence of the source brightness distribution. In the derived visibility function, we detect the signatures of an extended (Gaussian FWHM∼25mas) and a compact component (Gaussian FWHM∼5.8mas), with the compact component contributing about two-thirds of the total flux (both in H- and K-band). The brightness distribution is highly asymmetric, as indicated by the strong closure phases (up to ∼40°) and the detected position angle dependence of the visibilities and closure phases. To interpret these asymmetries, we employ various geometric as well as physical models, including a binary model, a skewed ring model, and a puffed-up inner rim model with a vertical or curved rim shape. For the binary and vertical rim model, no acceptable fits could be obtained. On the other hand, the skewed ring model and the curved puffed-up inner rim model allow us to simultaneously reproduce the measured visibilities and closure phases. From these models we derive the location of the dust sublimation radius (∼0.4AU), the disk inclination angle (∼35°), and a north-south disk orientation (PA∼180-190°). Our curved puffed-up rim model can reproduce reasonably well the interferometric observables and the SED and suggests a luminosity of ∼29L and the presence of relatively large (>1.2µm) Silicate dust grains. Our study also reveals discrepancies between the measured interferometric observables and the puffed-up inner rim models, providing important constraints for future refinements of these theoretical models. Perpendicular to the disk, two bow shock-like structures appear in the associated reflection nebula NGC6729, suggesting that the detected sub-AU size disk is the driving engine of a large-scale outflow. Detecting, for the first time, strong non-localized asymmetries in the inner regions of a Herbig Ae disk, our study supports the existence of a puffed-up inner rim in YSO disks.

Abstract Copyright:

Journal keyword(s): stars: pre-main-sequence - circumstellar matter - accretion, accretion disks - planetary systems: protoplanetary disks - planetary systems: formation - techniques: interferometric

Simbad objects: 22

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Number of rows : 22

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 951 2
2 HD 45677 Be* 06 28 17.4219761127 -13 03 11.130589443 7.86 8.52 8.50 8.11 8.01 B2IV/V[e] 307 0
3 HD 101328 * 11 39 22.9987659115 -51 25 28.665369485   9.00 7.42     K4III 10 0
4 HD 104479 * 12 01 44.5748117292 -69 11 52.411958188   8.22 6.96     K0III 11 0
5 HD 106248 * 12 13 56.4621438773 -78 34 26.173744076   7.593 6.337     K2/3IIICNII 18 0
6 HD 108570 PM* 12 28 33.5941550678 -56 24 28.141229129   7.07 6.13     K0/1III 28 0
7 * bet Cru bC* 12 47 43.26877 -59 41 19.5792 0.03 1.02 1.25 1.38 1.64 B1IV 325 0
8 HD 121384 PM* 13 56 32.9456961015 -54 42 16.804388911   6.78 6.01     G8VCH+0.3CaIwk 90 0
9 HD 135452 * 15 16 32.3672836089 -39 33 39.412481634   8.36 6.85     K3III 9 0
10 HD 145921 * 16 15 23.9575099918 -42 53 57.928839708   7.262 6.135     K2III 21 0
11 * 22 Oph * 16 54 50.8117261882 -23 30 44.463947646   7.70 6.75     G8IIICNII 12 0
12 EM* MWC 297 Ae* 18 27 39.5266257570 -03 49 52.136526892 15.57 14.34 12.31 11.34   B1.5Ve 270 0
13 HD 170499 * 18 30 53.6674235265 -27 57 06.320324920   9.58 7.73     K4III 11 0
14 HD 174631 * 18 52 37.0466269414 -29 22 46.837115906   7.441 6.098     K1III 15 0
15 NGC 6729 ISM 19 01 46.4 -36 57 40           ~ 54 0
16 V* R CrA Ae* 19 01 53.6850227874 -36 57 08.145519972 12.781 12.651 11.917 11.242 10.412 B5IIIpe 456 1
17 NAME Coronet Cluster Cl* 19 01 54 -36 57.2           ~ 82 1
18 2MASS J19015545-3657231 Y*O 19 01 55.460 -36 57 23.13           ~ 91 2
19 HH 104A * 19 01 58.95 -36 57 17.1           ~ 17 0
20 * lam Aql PM* 19 06 14.9397099975 -04 52 57.231496924 3.07 3.34 3.43 3.46 3.55 B8.5V 211 0
21 HD 181110 * 19 20 47.3154788856 -38 44 46.828608189   8.79 7.26     K3III 15 0
22 HD 183925 * 19 33 03.1596590070 -30 21 46.049526789   8.34 6.75     K5III 9 0

    Equat.    Gal    SGal    Ecl

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