Protoplanetary Disk Evolution: Singles vs. Binaries

Abstract

Abstract. Based on a large number of observations carried out in the last decade it appears that the fraction of stars with protoplanetary disks declines steadily between ∼1 Myr and ∼10 Myr. We do, however, know that the multiplicity fraction of star-forming regions can be as high as >50% and that multiples have reduced disk lifetimes on average. As a consequence, the observed roughly exponential disk decay can be fully attributed neither to single nor binary stars and its functional form may need revision. Observational evidence for a non-exponential decay has been provided by Kraus et al. (2012), who statistically correct previous disk frequency measurements for the presence of binaries and find agreement with models that feature a constantly high disk fraction up to ∼3 Myr, followed by a rapid ( 2 Myr) decline.We present results from our high angular resolution observational program to study the fraction of protoplanetary disks of single and binary stars separately. We find that disk evolution timescales of stars bound in close binaries (<100 AU) are significantly reduced compared to wider binaries. The frequencies of accretors among single stars and wide binaries appear indistinguishable, and are found to be lower than predicted from planet forming disk models governed by viscous evolution and photoevaporation.

A Herschel View of Protoplanetary Disks in the Σ Ori Cluster

“…The fraction of binary companions in young regions can be ∼30% or larger where close (< 100 AU) binaries can affect the evolution of protoplanetary and circumbinary disks by significantly reducing their lifetime (Daemgen et al 2015). In Taurus star-forming region the disk population affected by multiplicity constitutes close binaries with separations <40 AU (Kraus & Hillenbrand 2012).…”