Cavities in inner disks: the GM Aurigae case

Free access article

Issue		A&A Volume 490, Number 2, November I 2008


Page(s)		L15 - L18
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:200810732
Published online		01 October 2008

A&A 490, L15-L18 (2008)
DOI: 10.1051/0004-6361:200810732

Letter

Cavities in inner disks: the GM Aurigae case

A. Dutrey¹, S. Guilloteau¹, V. Piétu², E. Chapillon^{1, 2}, F. Gueth², T. Henning³, R. Launhardt³, Y. Pavlyuchenkov³, K. Schreyer⁴, and D. Semenov³

¹ LAB, UMR 5804, Observatoire de Bordeaux, 2 rue de l'Observatoire, 33270 Floirac, France
    e-mail: [Anne.Dutrey;Stephane.Guilloteau;edwige.chapillon]@obs.u-bordeaux1.fr
² IRAM, 300 rue de la Piscine, 38400 Saint Martin d'Hères, France
    e-mail: [pietu;gueth]@iram.fr
³ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
    e-mail: [henning;pavyar;semenov]@mpia.de; rl@mpia-hd.mpg.de
⁴ Astrophysikalisches Institut und Universitäts-Sternwarte, Schillergässchen 2-3, 07745 Jena, Germany
    e-mail: martin@astro.uni-jena.de

Received 1 August 2008 / Accepted 22 September 2008

Abstract
Context. Recent modeling based on unresolved infrared observations of the spectral energy distribution (SED) of GM Aurigae suggests that the inner disk of this single TTauri star is truncated at an inner radius of 25 AU.
Aims. We attempt to find evidence of this inner hole in the gas distribution, using spectroscopy with high angular resolution.
Methods. Using the IRAM array, we obtained high angular resolution (~1.5”) observations with a high S/N per channel of the ¹³CO J=2-1 and C¹⁸O J=2-1 and of the ¹³CO J=1-0 lines. A standard parametric disk model is used to fit the line data in the Fourier-plane and to derive the CO disk properties. Our measurement is based on a detailed analysis of the spectroscopic profile from the CO disk rotating in Keplerian velocity. The millimeter continuum, tracing the dust, is also analyzed.
Results. We detect an inner cavity of radius 19 $\pm$ 4 AU at the 4.5 $\sigma$ level. The hole manifests itself by a lack of emission beyond the (projected) Keplerian speed at the inner radius. We also constrain the temperature gradient in the disk.
Conclusions. Our data reveal the existence of an inner hole in GM Aur gas disk. Its origin remains unclear, but can be linked to planet formation or to a low mass stellar companion orbiting close to the central star (~5-15 AU). The frequent finding of inner cavities suggests that either binarity is the most common scenario of star formation in Taurus or that giant planet formation starts early.

Key words: stars: formation -- ISM: molecules -- stars: circumstellar matter -- radio lines: stars -- stars: individual: GM Aurigae

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