Protoplanetary disk evolution and stellar parameters of T Tauri binaries in Chamaeleon I^⋆,⋆⋆

¹ European Southern Observatory, Karl-Schwarzschildstr. 2, 85748 Garching, Germany
² Department of Astronomy & Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON M5S 3H4, Canada
e-mail: daemgen@astro.utoronto.ca
³ Institute for Astronomy, University of Hawaii, 34 Ohia Ku Street, Pukalani HI 96768, USA
⁴ Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
⁵ Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
⁶ Institut für Astronomie & Astrophysik, Universität Tübingen, Auf der Morgenstelle 10, 72076 Tübingen, Germany
⁷ SOFIA Science Center, NASA-Ames Research Center, MS 232-12, Moffett Field, CA 94035, USA
⁸ Deutsches SOFIA Institut, Univ. Stuttgart, Pfaffenwaldring 29, 70569 Stuttgart, Germany

Received: 1 February 2013
Accepted: 22 March 2013

Abstract

Aims. This study aims to determine the impact of stellar binary companions on the lifetime and evolution of circumstellar disks in the Chamaeleon I (Cha I) star-forming region by measuring the frequency and strength of accretion and circumstellar dust signatures around the individual components of T Tauri binary stars.

Methods. We used high-angular resolution adaptive optics JHK_sL′ -band photometry and 1.5–2.5 μm spectroscopy of 19 visual binary and 7 triple stars in Cha I – including one newly discovered tertiary component – with separations between ~25 and ~1000 AU. The data allowed us to infer stellar component masses and ages and, from the detection of near-infrared excess emission and the strength of Brackett-γ emission, the presence of ongoing accretion and hot circumstellar dust of the individual stellar components of each binary.

Results. Of all the stellar components in close binaries with separations of 25–100 AU, 10⁺¹⁵_-5% show signs of accretion. This is less than half of the accretor fraction found in wider binaries, which itself appears significantly reduced (~44%) compared with previous measurements of single stars in Cha I. Hot dust was found around 50⁺³⁰_-15% of the target components, a value that is indistinguishable from that of Cha I single stars. Only the closest binaries (<25 AU) were inferred to have a significantly reduced fraction (≲25%) of components that harbor hot dust. Accretors were exclusively found in binary systems with unequal component masses M_secondary/M_primary < 0.8, implying that the detected accelerated disk dispersal is a function of mass-ratio. This agrees with the finding that only one accreting secondary star was found, which is also the weakest accretor in the sample.

Conclusions. The results imply that disk dispersal is more accelerated the stronger the dynamical disk truncation, i.e., the smaller the inferred radius of the disk. Nonetheless, the overall measured mass accretion rates appear to be independent of the cluster environment or the existence of stellar companions at any separation ≳25 AU, because they agree well with observations from our previous binary study in the Orion Nebula cluster and with studies of single stars in these and other star-forming regions.