Issue |
A&A
Volume 564, April 2014
|
|
---|---|---|
Article Number | A118 | |
Number of page(s) | 7 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361/201322997 | |
Published online | 15 April 2014 |
The inner circumstellar disk of the UX Orionis star V1026 Scorpii ⋆,⋆⋆
1
Max-Planck-Institut für Radioastronomie,
Auf dem Hügel 69, 53121
Bonn,
Germany
e-mail:
jvural@mpifr-bonn.mpg.de
2
University of Exeter, Astrophysics group, Physics Building
Stocker Road Exeter, EX4 4QL, UK
3
Laboratoire Lagrange, UMR 7293, Université de Nice
Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, 06300
Nice,
France
4
UJF-Grenoble 1/CNRS-INSU, Institut de Planétologie et
d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041
Grenoble,
France
5
INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi,
5, 50125
Firenze,
Italy
Received:
6
November
2013
Accepted:
20
February
2014
Context. The UX Ori type variables (named after the prototype of their class) are intermediate-mass pre-main sequence objects. One of the most likely causes of their variability is the obscuration of the central star by orbiting dust clouds.
Aims. We investigate the structure of the circumstellar environment of the UX Ori star V1026 Sco (HD 142666) and test whether the disk inclination is large enough to explain the UX Ori variability.
Methods. We observed the object in the low-resolution mode of the near-infrared interferometric VLTI/AMBER instrument and derived H- and K-band visibilities and closure phases. We modeled our AMBER observations, published Keck Interferometer observations, archival MIDI/VLTI visibilities, and the spectral energy distribution using geometric and temperature-gradient models.
Results. Employing a geometric inclined-ring disk model, we find a ring radius of 0.15 ± 0.06 AU in the H band and 0.18 ± 0.06 AU in the K band. The best-fit temperature-gradient model consists of a star and two concentric, ring-shaped disks. The inner disk has a temperature of 1257+133-53 K at the inner rim and extends from 0.19 ± 0.01 AU to 0.23 ± 0.02 AU. The outer disk begins at 1.35+0.19-0.20 AU and has an inner temperature of 334+35-17 K. The derived inclination of 48.6+2.9-3.6° approximately agrees with the inclination derived with the geometric model (49 ± 5° in the K band and 50 ± 11° in the H band). The position angle of the fitted geometric and temperature-gradient models are 163 ± 9° (K band; 179 ± 17° in the H band) and 169.3+4.2-6.7°, respectively.
Conclusions. The narrow width of the inner ring-shaped model disk and the disk gap might be an indication for a puffed-up inner rim shadowing outer parts of the disk. The intermediate inclination of ~50° is consistent with models of UX Ori objects where dust clouds in the inclined disk obscure the central star.
Key words: stars: individual: V1026 Sco / stars: pre-main sequence / circumstellar matter / techniques: interferometric / accretion, accretion disks / stars: formation
© ESO, 2014
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