Sub-arcsec imaging of the AB Aur molecular disk and envelope at millimeter wavelengths: a non Keplerian disk
By V. Pi'etu, S. Guilloteau, A. Dutrey. 2005
147 citations recorded by the source corpus.
We present sub-arcsecond images of AB Auriga obtained with the IRAM Plateau de Bure interferometer in the isotopologues of CO, and in continuum at 3 and 1.3 mm. Instead of being centrally peaked, the continuum emission is dominated by a bright, asymmetric (spiral-like) feature at about 140 AU from the central star. The large scale molecular structure suggests the AB Aur disk is inclined between 23 and 43 degrees, but the strong asymmetry of the continuum and molecular emission prevents an accurate determination of the inclination of the inner parts. We find significant non-Keplerian motion, with a best fit exponent for the rotation velocity law of 0.41 +/- 0.01, but no evidence for radial motions. The disk has an inner hole about 70 AU in radius. The disk is warm and shows no evidence of depletion of CO. The dust properties suggest the dust is less evolved than in typical T Tauri disks. Both the spiral-like feature and the departure from purely Keplerian motions indicates the AB Aur disk is not in quasi-equilibrium. Disk self-gravity is insufficient to create the perturbation. This behavior may be related either to an early phase of star formation in which the Keplerian regime is not yet fully established and/or to a disturbance of yet unknown origin. An alternate, but unproven, possibility is that of a low mass companion located about 40 AU from AB Aur.
Subfields: Astronomy and Astrophysics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/ec7d1072ae05882340ad8bbe05dd8a6f3a74ea76
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 Instrumentation
Citations in the corpus
- Resolving the inner dust disks surrounding LkCa 15 and MWC 480 at mm wavelengths (2006, methodology): “IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). a large inner radius (70 – 100 AU) was measured in the mm domain for the dense spiral-like structure found in AB Auriga (Piétu et al. 2005).”
- Resolved gas cavities in transitional disks inferred from CO isotopologs with ALMA (2015, background): “For a handful of disks, pioneering interferometers such as SMA and PdBI have revealed gas inside the cavity through CO rotational lines: AB Aur (Piétu et al. 2005), GM Aur (Dutrey et al. 2008), and HD 135344B (Lyo et al. 2011).”
- PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, background): “…sensitivity and resolution have shown that this power-law+cut-off behavior yields inconsistent results for the location of Rout: the optically thin continuum emission indicates a significantly smaller Rout than the optically thick molecular line emission (Piétu et al. 2005; Isella et al. 2007).”
- Millimeter imaging of HD 163296: probing the disk structure and kinematics (2007, background): “A similar difference in the dust and gas outer radii has been also reported by Piétu et al. (2005) for the Herbig Ae star AB Aur.”
- Gas and Dust Emission at the Outer Edge of Protoplanetary Disks (2008, background): “…for the disparate outer radii observed using different probes of the disk extent, including comparison of continuum and molecular gas observations (Piétu et al. 2005; Isella et al. 2007), and also comparison of different isotopologues and rotational transitions of a particular molecule (Piétu…”
- THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, unknown): “A few studies used simple models to fit the millimeter continuum (dust) and CO line (gas) emission independently, finding inconsistent structures where the dust is much more compact than the gas (Piétu et al. 2005; Isella et al. 2007).”
- DIRECT IMAGING OF FINE STRUCTURES IN GIANT PLANET-FORMING REGIONS OF THE PROTOPLANETARY DISK AROUND AB AURIGAE (2011, background): “Note, however, that the optically thin submillimeter continuum radiation also reveals some of the arms; the spirals are not simply surface corrugation but also reflect the structures near the midplane of the disk (Lin et al. 2006; Piétu et al. 2005).”
- STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, background): “…been demonstrated that the power law parameterization fails to explain the differences in the radial extensions of the dust and the gas emission that are observed in a number of intermediate mass pre-main sequence stars (Piétu et al. 2005; Isella et al. 2007; Hughes et al. 2008, hereafter H08).”
- A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties (2011, background): “For LkCa 15 and GM Aur, we assumed no central hole for this comparison, and thus obtain different results from those in Table 5.”
- THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS (2013, unknown): “…Looney et al. 2000; Duvert et al. 2000; Motte & André 2001; Klein et al. 2003; Jensen & Akeson 2003; Duchêne et al. 2003, 2010; Corder et al. 2005; Piétu et al. 2005, 2006, 2011; Lin et al. 2006; Moriarty-Schieven et al. 2006; Scholz et al. 2006; Hamidouche et al. 2006; Andrews &…”
- Probing the structure of protoplanetary disks: a comparative study of DM Tau, LkCa 15, and MWC 480 (2007, methodology): “From Table 1 of Piétu et al. (2005), the13CO surface density in AB Aur at 300 AU is about 2 1016 cm−2, 4 to 8 times larger than in the DM Tau, MWC 480 or LkCa 15 disks.”
- Dust Evolution and the Formation of Planetesimals (2016, background): “Though succeeding in explaining many observed properties of disks, the power-law form for surface density profiles in disks hardly reconcile the observational fact that disk sizes from CO rotational line emission are much larger than those from dust emission (Piétu et al. 2005; Panić et al. 2009).”