Emission Lines from the Gas Disk around TW Hydra and the Origin of the Inner Hole

Details Emission Lines from the Gas Disk around TW Hydra and the Origin of the Inner Hole Emission Lines from the Gas Disk around TW Hydra and the Origin of the Inner Hole

2011-04-25

arxiv.org/abs/1104.4806v1

Astronomy and Astrophysics

Astrophysics

Earth and Planetary Astrophysics

To appear in the Astrophysical Journal

Scientific paper

We compare line emission calculated from theoretical disk models with optical to sub-millimeter wavelength observational data of the gas disk surrounding TW Hya and infer the spatial distribution of mass in the gas disk. The model disk that best matches observations has a gas mass ranging from $\sim10^{-4}-10^{-5}$\ms\ for $0.06{\rm AU} 13.6$eV) flux from TW Hya. H$_2$ pure rotational line emission comes primarily from $r\sim 1-30$AU. [OI]63$\mu$m, HCO$^+$ and CO pure rotational lines all arise from the outer disk at $r\sim30-120$AU. We discuss planet formation and photoevaporation as causes for the decrease in surface density of gas and dust inside 4 AU. If a planet is present, our results suggest a planet mass $\sim 4-7$M$_J$ situated at $\sim 3$AU. Using our photoevaporation models and the best surface density profile match to observations, we estimate a current photoevaporative mass loss rate of $4\times10^{-9}$\ms\ yr$^{-1}$ and a remaining disk lifetime of $\sim 5$ million years.

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