  HD 135344B is an accreting (pre-) transition disk that displays the emission
of warm CO extending tens of AU inside its 30 AU dust cavity. We used the dust
radiative transfer code MCFOST and the thermochemical code ProDiMo to derive
the disk structure from the simultaneous modeling of the spectral energy
distribution (SED), VLT/CRIRES CO P(10) 4.75 micron, Herschel/PACS [O I] 63
micron, Spitzer-IRS, and JCMT 12CO J=3-2 spectra, VLTI/PIONIER H-band
visibilities, and constraints from (sub-)mm continuum interferometry and
near-IR imaging. We found a disk model able to describe the current
observations simultaneously. This disk has the following structure. (1) To
reproduce the SED, the near-IR interferometry data, and the CO ro-vibrational
emission, refractory grains (we suggest carbon) are present inside the silicate
sublimation radius (0.08<R<0.2 AU). (2) The dust cavity (R<30 AU) is filled
with gas, the surface density of this gas must increase with radius to fit the
CO P(10) line profile, a small gap of a few AU in the gas is compatible with
current data, and a large gap in the gas is not likely. (4) The gas/dust ratio
inside the cavity is > 100 to account for the 870 micron continuum upper limit
and the CO P(10) line flux. (5) The gas/dust ratio at 30<R<200 AU is < 10 to
simultaneously describe the [O I] 63 micron line flux and the CO P(10) line
profile. (6) In the outer disk, most of the mass should be located in the
midplane, and a significant fraction of the dust is in large grains.
Conclusions: Simultaneous modeling of the gas and dust is required to break the
model degeneracies and constrain the disk structure. An increasing gas surface
density with radius in the inner dust cavity echoes the effect of a migrating
Jovian planet. The low gas mass (a few MJupiter) in the HD 135344B's disk
suggests that it is an evolved disk that has already lost a large portion of
its mass.

Solar and Stellar Astrophysics