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Untitled - Laboratoire d'Astrophysique de l'Observatoire de Grenoble

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Figure 6.3: Contribution of heating processes in a T Tauri disk: radial profile of these contributions to the temperature<br />

of the disk. Left: mid-plane temperature, middle: effective temperature, right: surface temperature.<br />

One sees that in the inner 2 AUs the mid-plane temperature is dominated by the viscous dissipation. From<br />

Lachaume et al. (2003).<br />

IOTA and VLTI/VINCI.<br />

Figure 6.4: FU Orionis disk-spot mo<strong>de</strong>l. Lines corresponds to the best mo<strong>de</strong>l fit and markers to visibilities in<br />

binned form. Top-left panel: spectral energy distribution and best fit mo<strong>de</strong>l. The solid line stands for the whole<br />

mo<strong>de</strong>l and the dashed one for the spot. Right panel: visibility data vs. hour angle for each baseline in H and<br />

K. The contribution of the disk is displayed in dashed lines. Bottom-left panel: synthetic image in logarithmic<br />

scale. East is left and North is up. From Malbet et al. (2005).<br />

FU Ori was observed on 42 nights over a period of 6 years, from 1998 to 2003. 287 in<strong>de</strong>pen<strong>de</strong>nt measurements<br />

of the fringe visibility with 6 different baselines ranging from 20 to 110m, in the H- and K-bands, were obtained,<br />

see Fig. 6.4. Our data resolve FU Ori at the AU scale, and provi<strong>de</strong>s new constraints at shorter baselines and<br />

shorter wavelengths. Our extensive (u,v)-plane coverage, coupled with the published spectral energy distribution<br />

data shows that FU Ori hosts an active accretion disk whose temperature law is consistent with standard<br />

mo<strong>de</strong>ls. A 10% peak-to-peak oscillation is <strong>de</strong>tected in the longest baseline data. It is interpreted as a possible<br />

disk hot-spot or companion. Although this bright spot on the surface of the disk could be tracing some thermal<br />

instabilities in the disk, we have proposed to interpret this spot as the signature of a companion of the central FU<br />

Ori system on an extremely eccentric orbit. We speculate that the close encounter of this putative companion<br />

and the central star could be the explanation of the initial photometric rise of the luminosity of this object.<br />

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