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The circumstellar environment of UX Ori *
A. Natta 1,
T. Prusti 2,
R. Neri 3,
W.F. Thi 4,
V.P. Grinin 5,6 and
V. Mannings 7
Received 7 June 1999 / Accepted 30 July 1999
This paper presents new observations of UX Ori obtained with the millimeter interferometer of Plateau de Bure and with ISO. UX Ori is the prototype of a group of pre-main-sequence, intermediate-mass stars, often indicated as precursors of Pic. The interferometry observations at 1.2 and 2.6 mm show that UX Ori has a circumstellar disk, with outer radius AU. We determine the spectral index between these two wavelengths to be 2.10.2, consistent with the disk being optically thick at mm wavelengths. Alternatively, the disk solid matter can be in the form of "pebbles" (radius10 cm). In both cases most of the disk mass must be in gas form, and small grains must be present, at least in the disk atmosphere. In both cases also, the disk must be rather massive ( 0.1 ). The existence of a circumstellar disk supports the model of the UXOR phenomenon in terms of a star+disk system. Self-consistent models of almost edge-on disks account well for the observed emission at all wavelengths longer than about 8µm, if we include the emission of the optically thin, superheated layers that enshroud the disk. These rather simple disk models fail to account for the strong emission observed in the near-IR (i.e., between and 7 µm), and we suggest a number of possible explanations.
Key words: stars: circumstellar matter stars: formation stars: individual: UX Ori
* Based in part on observations obtained with ISO. ISO is an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA.
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Online publication: October 4, 1999