A model exploration of NIR ro-vibrational CO emission as a tracer of inner cavities in protoplanetary disks. (arXiv:2003.11788v1 [astro-ph.SR])

A model exploration of NIR ro-vibrational CO emission as a tracer of inner cavities in protoplanetary disks. (arXiv:2003.11788v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Antonellini_S/0/1/0/all/0/1">S. Antonellini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banzatti_A/0/1/0/all/0/1">A. Banzatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kamp_I/0/1/0/all/0/1">I. Kamp</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Thi_W/0/1/0/all/0/1">W.-F. Thi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Woitke_P/0/1/0/all/0/1">P. Woitke</a>

Near-IR observations of protoplanetary disks provide information about the
properties of the inner disk. High resolution spectra of abundant molecules
such as CO can be used to determine the disk structure in the warm inner parts.
The $v2/v1$ ro-vibrational ratio of $v_{1-0}$ and $v_{2-1}$ transitions has
been recently observed to follow distinct trends with the CO emitting radius,
in a sample of TTauri and Herbig disks; these trends have been empirically
interpreted as due to inner disk depletion from gas and dust. In this work we
use existing thermo-chemical disk models to explore the interpretation of these
observed trends in ro-vibrational CO emission. We use the radiation
thermo-chemical code ProDiMo, exploring a set of previously published models
with different disk properties and varying one parameter at a time: the inner
radius, the dust-to-gas mass ratio, the gas mass. In addition, we use models
where we change the surface density power law index, and employ a larger set of
CO ro-vibrational levels, including also fluorescence from the first electronic
state. We investigate these models for both TTauri and Herbig star disks.
Finally, we include a set of DIANA models for individual TTauri and Herbig
disks which were constructed to reproduce a large set of multi-wavelength
observations.

Near-IR observations of protoplanetary disks provide information about the
properties of the inner disk. High resolution spectra of abundant molecules
such as CO can be used to determine the disk structure in the warm inner parts.
The $v2/v1$ ro-vibrational ratio of $v_{1-0}$ and $v_{2-1}$ transitions has
been recently observed to follow distinct trends with the CO emitting radius,
in a sample of TTauri and Herbig disks; these trends have been empirically
interpreted as due to inner disk depletion from gas and dust. In this work we
use existing thermo-chemical disk models to explore the interpretation of these
observed trends in ro-vibrational CO emission. We use the radiation
thermo-chemical code ProDiMo, exploring a set of previously published models
with different disk properties and varying one parameter at a time: the inner
radius, the dust-to-gas mass ratio, the gas mass. In addition, we use models
where we change the surface density power law index, and employ a larger set of
CO ro-vibrational levels, including also fluorescence from the first electronic
state. We investigate these models for both TTauri and Herbig star disks.
Finally, we include a set of DIANA models for individual TTauri and Herbig
disks which were constructed to reproduce a large set of multi-wavelength
observations.

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