Duchêne, G.; McCabe, C.; Pinte, C.; Stapelfeldt, K. R.; Ménard, F.; Duvert, G.; Ghez, A. M.; Maness, H. L.; Bouy, H.; Barrado y Navascués, D.; Morales-Calderón, M.; Wolf, S.; Padgett, D. L.; Brooke, T. Y.; Noriega-Crespo, A.
Referencia bibliográfica
The Astrophysical Journal, Volume 712, Issue 1, pp. 112-129 (2010).
Fecha de publicación:
3
2010
Revista
Número de citas
57
Número de citas referidas
52
Descripción
We present new high spatial resolution (lsim0farcs1) 1-5 μm adaptive
optics images, interferometric 1.3 mm continuum and 12CO 2-1
maps, and 350 μm, 2.8 and 3.3 mm fluxes measurements of the HV Tau
system. Our adaptive optics images unambiguously demonstrate that HV Tau
AB-C is a common proper motion pair. They further reveal an unusually
slow orbital motion within the tight HV Tau AB pair that suggests a
highly eccentric orbit and/or a large deprojected physical separation.
Scattered light images of the HV Tau C edge-on protoplanetary disk
suggest that the anisotropy of the dust scattering phase function is
almost independent of wavelength from 0.8 to 5 μm, whereas the dust
opacity decreases significantly over the same range. The images further
reveal a marked lateral asymmetry in the disk that does not vary over a
timescale of two years. We further detect a radial velocity gradient in
the disk in our 12CO map that lies along the same position
angle as the elongation of the continuum emission, which is consistent
with Keplerian rotation around a 0.5-1 M sun central star,
suggesting that it could be the most massive component in the triple
system. To obtain a global representation of the HV Tau C disk, we
search for a model that self-consistently reproduces observations of the
disk from the visible regime up to millimeter wavelengths. We use a
powerful radiative transfer model to compute synthetic disk observations
and use a Bayesian inference method to extract constraints on the disk
properties. Each individual image, as well as the spectral energy
distribution, of HV Tau C can be well reproduced by our models with
fully mixed dust provided grain growth has already produced
larger-than-interstellar dust grains. However, no single model can
satisfactorily simultaneously account for all observations. We suggest
that future attempts to model this source include more complex dust
properties and possibly vertical stratification. While both grain growth
and stratification have already been suggested in many disks, only a
panchromatic analysis, such as presented here, can provide a complete
picture of the structure of a disk, a necessary step toward
quantitatively testing the predictions of numerical models of disk
evolution.
Data presented in this study were obtained during the course of ESO
program 70.C-0565 and IRAM program O048.