The unusual protoplanetary disk around the T Tauri star ET Chamaeleontis

Abstract

We present new continuum and line observations, along with modelling, of the faint (6−8) Myr old T Tauri star ET Cha belonging to the η Chamaeleontis cluster. We have acquired Herschel/PACS photometric fluxes at 70 μm and 160 μm, as well as a detection of the [OI] 63 μm fine-structure line in emission, and derived upper limits for some other far-IR OI, CII, CO and o-H 2 O lines. These observations were carried out in the frame of the open time key programme GASPS, where ET Cha was selected as one of the science demonstration phase targets. The Herschel data is complemented by new simultaneous ANDICAM B−K photometry, new HST/COS and HST/STIS UV-observations, a non-detection of CO J = 3 → 2 with APEX, re-analysis of a UCLES high-resolution optical spectrum showing forbidden emission lines like [OI] 6300 Å, [SII] 6731 Å and 6716 Å, and [NII] 6583 Å, and a compilation of existing broad-band photometric data. We used the thermo-chemical disk code ProDiMo and the Monte-Carlo radiative transfer code MCFOST to model the protoplanetary disk around ET Cha. The paper also introduces a number of physical improvements to the ProDiMo disk modelling code concerning the treatment of PAH ionisation balance and heating, the heating by exothermic chemical reactions, and several non-thermal pumping mechanisms for selected gas emission lines. By applying an evolutionary strategy to minimise the deviations between model predictions and observations, we find a variety of united gas and dust models that simultaneously fit all observed line and continuum fluxes about equally well. Based on these models we can determine the disk dust mass with confidence, M dust ≈ (2−5) × 10 −8 M whereas the total disk gas mass is found to be only little constrained, M gas ≈ (5 × 10 −5 −3 × 10 −3 ) M . Both mass estimates are substantially lower than previously reported. In the models, the disk extends from 0.022 AU (just outside of the co-rotation radius) to only about 10 AU, remarkably small for single stars, whereas larger disks are found to be inconsistent with the CO J = 3 → 2 non-detection. The low velocity component of the [OI] 6300 Å emission line is centred on the stellar systematic velocity, and is consistent with being emitted from the inner disk. The model is also consistent with the line flux of H 2 v = 1 → 0 S(1) at 2.122 μm and with the [OI] 63 μm line as seen with Herschel/PACS. An additional high-velocity component of the [OI] 6300 Å emission line, however, points to the existence of an additional jet/outflow of low velocity 40−65 km s −1 with mass loss rate ≈10 −9 M /yr. In relation to our low estimations of the disk mass, such a mass loss rate suggests a disk lifetime of only ∼0.05−3 Myr, substantially shorter than the cluster age. If a generic gas/dust ratio of 100 was assumed, the disk lifetime would be even shorter, only ∼3000 yrs. The evolutionary state of this unusual protoplanetary disk is discussed.

The Taurus Boundary of Stellar/Substellar (TBOSS) Survey

“…While the new and known transition disks have a distinct distribution in the slope over the 24 µm to 70 µm range, the spectral indices for these objects at longer wavelengths are indistinguishable from the values for the general Class II population. Another set of 8 targets have very steep SED slopes over the 24 µm to 70 µm range, possibly indicating truncated disks such as has been suggested for the disk around ET Cha (Woitke et al 2011). Two other unusual targets are diskbearing secondary components of mixed systems.…”

“…An example of a likely truncated disk in the Cha moving group around ET Cha was identified from a similarly steep SED index (α 24−70 µm = −1.4) over wavelengths extending to the PACS bands combined with a non-detection of the CO(3-2) line (Woitke et al 2011). In addition to the 3 Class II non-detected sources, there are 5 Class II targets with 70 µm detections that also define a slope as steep as that of ET Cha -CFHT 12, FR Tau, KPNO 13, J04141188+2811535, and V410 Xray 1 -resulting in a total of 8 candidate truncated disks.…”

Consistent dust and gas models for protoplanetary disks

“…PAH freeze-out can modify the heating-cooling balance as well as the ionisation fraction in disks. The ionisation balance is calculated using the local UV radiation field (Woitke et al 2011). The models described in this paper use circumcoronene (C 54 H 18 ) as the representative PAH.…”

Stellar energetic particle ionization in protoplanetary disks around T Tauri stars

“…If not noted otherwise, these parameters are kept fixed for all our models presented in this work. For more details on the parameter definitions see Woitke et al (2009Woitke et al ( , 2011Woitke et al ( , 2016. (a) χ ISM is given in units of the Draine field (Draine & Bertoldi 1996;Woitke et al 2009).…”