Bouarour, Y. -I., Perraut, K., Menard, F., Brandner, W., Caratti o Garatti, A., Caselli, P., van Dishoeck, E., Dougados, C., Garcia-Lopez, R., Grellmann, R., Henning, T., Klarmann, L., Labadie, L., Natta, A., Sanchez-Bermudez, J., Thi, W. -F., de Zeeuw, P. T., Amorim, A., Baubock, M., Benisty, M., Berger, J. -P., Clenet, Y., du Foresto, V. Coude, Duvert, G., Eckart, A., Eisenhauer, F., Eupen, F., Filho, M., Gao, F., Garcia, P., Gendron, E., Genzel, R., Gillessen, S., Jimenez-Rosales, A., Jocou, L., Hippler, S., Horrobin, M., Hubert, Z., Kervella, P., Lacour, S., Le Bouquin, J. -B., Lena, P., Ott, T., Paumard, T., Perrin, G., Pfuhl, O., Rousset, G., Scheithauer, S., Shangguan, J., Stadler, J., Straub, O., Straubmeier, C., Sturm, E., Vincent, F. H., von Fellenberg, S. D., Widmann, F. and Wiest, M. (2020). The GRAVITY young stellar object survey: III. The dusty disk of RY Lup. Astron. Astrophys., 642. LES ULIS CEDEX A: EDP SCIENCES S A. ISSN 1432-0746

Full text not available from this repository.

Abstract

Context. Studies of the dust distribution, composition, and evolution of protoplanetary disks provide clues for understanding planet formation. However, little is known about the innermost regions of disks where telluric planets are expected to form.Aims. We aim constrain the geometry of the inner disk of the T Tauri star RY Lup by combining spectro-photometric data and interferometric observations in the near-infrared (NIR) collected at the Very Large Telescope Interferometer. We use PIONIER data from the ESO archive and GRAVITY data that were obtained in June 2017 with the four 8m telescopes.Methods. We use a parametric disk model and the 3D radiative transfer code MCFOST to reproduce the spectral energy distribution (SED) and match the interferometric observations. MCFOST produces synthetic SEDs and intensity maps at different wavelengths from which we compute the modeled interferometric visibilities and closure phases through Fourier transform.Results. To match the SED from the blue to the millimetric range, our model requires a stellar luminosity of 2.5 L-circle dot, higher than any previously determined values. Such a high value is needed to accommodate the circumstellar extinction caused by the highly inclined disk, which has been neglected in previous studies. While using an effective temperature of 4800 K determined through high-resolution spectroscopy, we derive a stellar radius of 2.29 R-circle dot. These revised fundamental parameters, when combined with the mass estimates available (in the range 1.3-1.5 M-circle dot), lead to an age of 0.5-2.0 Ma for RY Lup, in better agreement with the age of the Lupus association than previous determinations. Our disk model (that has a transition disk geometry) nicely reproduces the interferometric GRAVITY data and is in good agreement with the PIONIER ones. We derive an inner rim location at 0.12 au from the central star. This model corresponds to an inclination of the inner disk of 50 degrees, which is in mild tension with previous determinations of a more inclined outer disk from SPHERE (70 degrees in NIR) and ALMA (67 5 degrees) images, but consistent with the inclination determination from the ALMA CO spectra (55 +/- 5 degrees). Increasing the inclination of the inner disk to 70 degrees leads to a higher line-of-sight extinction and therefore requires a higher stellar luminosity of 4.65 L-circle dot to match the observed flux levels. This luminosity would translate to a stellar radius of 3.13 R-circle dot, leading to an age of 2-3 Ma, and a stellarmass of about 2 M-circle dot, in disagreement with the observed dynamical mass estimate of 1.3-1.5 M-circle dot. Critically, this high-inclination inner disk model also fails to reproduce the visibilities observed with GRAVITY.Conclusions. The inner dust disk, as traced by the GRAVITY data, is located at a radius in agreement with the dust sublimation radius. An ambiguity remains regarding the respective orientations of the inner and outer disk, coplanar and mildly misaligned, respectively.As our datasets are not contemporary and the star is strongly variable, a deeper investigation will require a dedicated multi-technique observing campaign.

Item Type: Journal Article
Creators:
CreatorsEmailORCIDORCID Put Code
Bouarour, Y. -I.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Perraut, K.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Menard, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Brandner, W.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Caratti o Garatti, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Caselli, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
van Dishoeck, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Dougados, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Garcia-Lopez, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Grellmann, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Henning, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Klarmann, L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Labadie, L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Natta, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Sanchez-Bermudez, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Thi, W. -F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
de Zeeuw, P. T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Amorim, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Baubock, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Benisty, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Berger, J. -P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Clenet, Y.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
du Foresto, V. CoudeUNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Duvert, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Eckart, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Eisenhauer, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Eupen, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Filho, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gao, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Garcia, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gendron, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Genzel, R.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Gillessen, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Jimenez-Rosales, A.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Jocou, L.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hippler, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Horrobin, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Hubert, Z.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Kervella, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lacour, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Le Bouquin, J. -B.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Lena, P.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Ott, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Paumard, T.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Perrin, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Pfuhl, O.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Rousset, G.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Scheithauer, S.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Shangguan, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Stadler, J.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Straub, O.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Straubmeier, C.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Sturm, E.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Vincent, F. H.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
von Fellenberg, S. D.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Widmann, F.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
Wiest, M.UNSPECIFIEDUNSPECIFIEDUNSPECIFIED
URN: urn:nbn:de:hbz:38-314848
DOI: 10.1051/0004-6361/202038249
Journal or Publication Title: Astron. Astrophys.
Volume: 642
Date: 2020
Publisher: EDP SCIENCES S A
Place of Publication: LES ULIS CEDEX A
ISSN: 1432-0746
Language: English
Faculty: Unspecified
Divisions: Unspecified
Subjects: no entry
Uncontrolled Keywords:
KeywordsLanguage
MAIN-SEQUENCE TRACKS; T-TAURI; RADIATIVE-TRANSFER; GASMultiple languages
Astronomy & AstrophysicsMultiple languages
URI: http://kups.ub.uni-koeln.de/id/eprint/31484

Downloads

Downloads per month over past year

Altmetric

Export

Actions (login required)

View Item View Item