Structure of the DM Tau Outer Disk: Probing the vertical kinetic temperature gradient

By E. Dartois, A. Dutrey, S. Guilloteau. 2003

209 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/59e5b6073e3c51ff7199418bbbad0b5167282402

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Spectroscopy

Citations in the corpus

A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO+ (2017, methodology): “The modeling code comes from Flaherty et al. (2015), which is based on earlier works by Rosenfeld et al. (2013) and Dartois et al. (2003).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES (2010, background): “…Andrews & Williams 2007a; Hughes et al. 2008; Isella et al. 2009), clearly established the presence of vertical temperature and density gradients (Dartois et al. 2003; Piétu et al. 2007), and even identified disks with large central cavities that exhibit very little dust emission (Piétu et al.…”
Photodesorption of ices I: CO, N₂, and CO₂ (2008, background): “Cold CO gas is also detected in the midplanes of protoplanetary disks (Dartois et al. 2003; Piétu et al. 2007) where the densities are higher and the freeze-out time scales are even shorter, suggesting the existence of either efficient non-thermal desorption or an efficient mixing process in the…”
Measuring turbulence in TW Hydrae with ALMA: methods and limitations (2016, methodology): “In the following we give a brief description of the parametric model but refer the reader to Dartois et al. (2003) and Piétu et al. (2007) for a thorough model description and fitting methodology.”
RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “Although the gas disk around this cool, young star in the Taurus clouds has been studied extensively (e.g., Guilloteau & Dutrey 1998; Dartois et al. 2003; Piétu et al. 2007), our new SMA observations permit the first sub-arcsecond resolution examination of the 880µm dust continuum emission.”
THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, methodology): “To be able to reproduce the observed CO spectral images, we have characterized the vertical temperature profile of the gas in parametric form, based on the modeling analysis of Dartois et al. (2003).”
A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties (2011, result): “In particular, the mass of the DM Tau disk becomes quite significant (0.2 M ) compared to the stellar mass (0.5 M Dartois et al. 2003).”
Millimeter imaging of HD 163296: probing the disk structure and kinematics (2007, methodology): “Piétu et al. (2007) have recently reported that for the HAe stars MWC 480 and AB Aur and the TTS DM Tau, the 12CO and 13CO lines are characterized by different temperatures, while in the case of the TTS LkCa 15 the CO temperatures are all similar.”
Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, methodology): “Observations of molecular lines are key to characterizing the distribution and dynamics of gas in disks (e.g., Dartois et al. 2003; Isella et al. 2007; Rosenfeld et al. 2012).”
A PARAMETRIC MODELING APPROACH TO MEASURING THE GAS MASSES OF CIRCUMSTELLAR DISKS (2013, methodology): “Following Dartois et al. (2003), we parameterize the atmospheric temperature as a radial power law in the same way as for the midplane profile, Tatm(r) = Tatm,1 ( r 1 AU )−q .”
Probing the structure of protoplanetary disks: a comparative study of DM Tau, LkCa 15, and MWC 480 (2007, methodology): “The13CO J=1-0 and J=21 observations of DM Tau are described in Dartois et al. (2003).”
Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations (2014, background): “It is assumed that the absolute value of this velocity component is on the order of 100 ms−1 (e.g., Dartois et al. 2003; Piétu et al. 2007; Hughes et al. 2011).”
Sub-arcsec imaging of the AB Aur molecular disk and envelope at millimeter wavelengths: a non Keplerian disk (2005, methodology): “Also, an independent constraint on the surface density and the temperature laws is no longer possible; for an optically thin J=1-0 line, the data only constrain the ratioΣ/T and the value ofp − q (Dartois et al. 2003).”
Direct mapping of the temperature and velocity gradients in discs Imaging the vertical CO snow line around IM Lupi (2017, background): “…from the scatter in line-free channels. modelling of multiple CO lines can provide an estimate of the vertical temperature structure of the disc (Dartois et al. 2003), indicate freeze-out of the gas phase molecules onto dust grains in the cold midplane (e.g. Qi et al. 2011; Zhang et al. 2017),…”
Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae (2005, methodology): “Surface densities from measured CO emission maps: In the case of DM Tau, measurements of 12CO, 13CO and C18O lines allow for a direct determination of the density profile of gaseous CO from orbital distances ∼ 100AU to the outer disk (Dartois et al. 2003).”
Survival of molecular gas in cavities of transition disks - I. CO (2013, background): “The reason why optically thick lines still slightly increase with δgas is, that the line can broaden or get optically thick higher in the disk, thus tracing warmer regions (van Zadelhoff et al. 2001; Dartois et al. 2003).”
Turbulence in the TW Hya Disk (2018, methodology): “The modeling code used to match the observations (CO(2-1)/CO(3-2)/CO(6-5) at ν=230.538 GHz, 345.79599 GHz, and 691.47308 GHz respectively) was used previously in Flaherty et al. (2015) and Flaherty et al. (2017) and is based on earlier work by Rosenfeld et al. (2013) and Dartois et al. (2003).”