The Impact of Multiplicity on Planet Formation Adam Kraus Hawaii-IfA Michael Ireland (Sydney), Frantz Martinache (Subaru), Lynne Hillenbrand (Caltech) Beta Pic CoKu Tau/4 LkHa 330

Canonical Model of Star Formation The canonical model of star formation (Shu et al. 1987)

Protoplanetary Disks as Sites of Ongoing Planet Formation CoKu Tau/4 (Model; Quillen et al. 2004) Transitional Disks Protoplanetary disks have large cleared gaps – perhaps signposts of planet formation? LkHa 330 (Submm image; Brown et al. 2008)

The Timescale for Planet Formation Disk Frequency as a Function of Age Haisch et al. (2001) The Disk dispersal timescale (~5 Myr) sets the timescale for possible planet formation.

Our Survey Most of our survey is being conducted with Keck using a new technique called aperture-mask interferometry. We could detect equal-brightness companions at ~1/4 λ/D (15 mas) and achieve the best sensitivity (ΔK~6) at ~λ/D (50 mas). We’ve observed ~100 members each for Taurus (T~2 Myr) and Upper Sco (T~5 Myr), spanning masses of M sun.

Aperture Mask Interferometry Placing an aperture mask in the pupil plane turn the single mirror into a sparse interferometric array. Interferometric analysis techniques (i.e. closure phases) can be used to filter almost all noise from turbulence and AO errors. This yields very stable performance. Our plan is to pursue a new planet- search strategy. We trade lower sensitivity (10 3 versus 10 6 ) for superior resolution (~λ/D versus 10λ/D), and then we observe distant young stars where substellar companions are much brighter.

Survey Results We found many new companions, but few with ΔK>3 and none with ΔK>4; a few might be substellar. Our limits extend to ΔK~6 at Keck. (Keck limits extend to ~8-15 M Jup for Upper Sco members or ~6-13 M Jup for Taurus members.) Red circles: Masking detections Crosses: Known binaries Dashed lines: 99.5% Detection Limits

The Disk around CoKu Tau/4 SED modeling suggests that the inner AU of the disk around CoKu Tau/4 have been cleared; this has been attributed this to active planet formation. We actually found that CoKu Tau/4 an ~8 AU binary; the disk truncation is therefore a natural result of tidal truncation and not planet formation. Troubling Question: Many of the other hosts for “transitional” disks haven’t been thoroughly surveyed for multiplicity. How many are actually circumbinary disks?

Circumbinary “transitional” disks? Detection limits (K-band multiplicity survey; solid lines) for GM Aur, UX Tau, LkCa15, and LkHa330 from Keck. Next step is a deep L-band survey of these targets to search for planetary-mass companions (dotted lines).

Circumbinary “transitional” disks? 20% of all solar-type stars appear to have 2-40 AU binary companions, so why don’t we see ~20 “fake” transitional disks in places like Taurus? Many of the disk-free stars in Taurus are turning out to be close binaries! (Hubble 4, LkCa4+5+21, V827 Tau, almost anything with CIDA in its name) This isn’t a new idea (Ghez et al. 1997; White & Ghez 2001; Cieza et al. 2008), but our survey is the first with enough resolution and sensitivity to study most of this separation range. But wait a minute…

Binaries and Disks The disk fraction as a function of separation for Taurus solar-type stars in binary systems. The disk location (primary, secondary, or circumbinary) hasn’t been determined for most systems).

Disk Lifetime in Close Binary Systems

The Multiplicity Correction It seems that many of the disk-free stars at 1- 2 Myr are binaries; if we remove them, the disk fraction of genuinely single stars goes up by ~15-20%. Under this picture, most circumstellar disks last at least 2-3 Myr; most circumbinary disks, on the other hand, seem to disperse promptly. (Disk fractions from Hillenbrand 2005).

Under this picture, most circumstellar disks last at least 1-2 Myr; most circumbinary disks, on the other hand, seem to disperse promptly. Numerous surveys have found that even circumstellar disks are mostly gone by 5 Myr, though. (Carpenter et al. 2006) Disk Lifetimes (Figure from Alexander & Armitage 2009)

Implications for Planet Formation Most single stars have >1-2 Myr within which to form planets (but not much more than 5). Close binary systems have <1 Myr. (This doesn’t bode well for planet searches around close binaries…) Note: There are variable outcomes. Judging by the SEDs, DP Tau has a full disk, CoKu Tau/4 has a circumbinary disk, and Hubble 4 has no disk. Why? Some binaries have long-lived disks; most seem to be in binary systems with equal mass components and/or circular orbits. (CoKuTau/4, ST 34, GG Tau, HD 98800)

Summary Some are close binaries, but they seem to be a small minority If disk gaps are cleared by companions, then most are planets. Some are close binaries, but they seem to be a small minority The majority of close (<40 AU) binaries lose their protoplanetary disks extremely quickly (<0.5 Myr). (alpha Cen, Sirius, Procyon, 61 Cyg…) The majority of close (<40 AU) binaries lose their protoplanetary disks extremely quickly (<0.5 Myr). Planets in close binary systems should be rare. (alpha Cen, Sirius, Procyon, 61 Cyg…) This prompt dispersal of circumbinary disks removes the need for prompt dispersal of circumstellar disks. This prompt dispersal of circumbinary disks removes the need for prompt dispersal of circumstellar disks. Most single stars and wide binaries have ~3 Myr to form planets (so why do only ~10% have gas giants?)