08:30 to 09:50 Registration 09:50 to 10:00 Welcome - Ben Mestel 10:00 to 11:00 L Hartmann ([Michigan])Review - protostellar disk observationsSession: 1 - Observations of Protoplanetary Discs Rapid progress is being made in developing observational constraints on the structure and evolution of protoplanetary disks, primarily due advances in spectral sensitivity due to the Spitzer Space Telescope and improvements in spatial resolution from mm-wave interferometry. Unfortunately there still are considerable uncertainties in the masses and mass distributions of disks. I will review the observational limits we now have on disk masses, the evidence for dust growth and settling in these disks, and the increasingly common indications of inner disk clearing at early evolutionary times (~ 1 Myr). I will then argue that the time-dependence of disk accretion in the protostellar phase strongly suggests that something like a dead zone or high-surface-density, low-viscosity, region exists in inner disks, at least initially, providing the conditions for more rapid formation of relatively massive bodies. 11:00 to 11:30 Coffee and posters INI 1 11:30 to 11:50 D Wilner ([Harvard Smithsonian Center])Submm observations of protoplanetary disksSession: 1 - Observations of Protoplanetary Discs Observations over a wide wavelength range provide diagnostic information on protoplanetary disks, but the submillimeter regime is especially important because (1) optically thin dust emission probes particles through the entire disk, including the cold midplane, (2) these are the longest wavelengths where dust is readily detectable, and therefore the last direct link on the chain of sizes from sub-micron interstellar particles to planetesimals, (3) aligned dust particles can produce polarized emission that traces the magnetic field, and (4) spectral line emission from a variety of species show the detailed disk kinematics and constrain nebular chemistry. I will describe recent results from the Submillimeter Array that take advantage of several of these key features, with implications for disk structure, planet forming potential, and the physics of accretion. In particular, I will discuss a high resolution (0.3 arcsec = 40 AU) 870 micron survey of dust continuum emission from young disks in the Ophiuchus star-forming region, where we have used 2D radiative transfer calculations to fit simultaneously the resolved submillimeter data and the broadband spectral energy distributions with a parametric model in an effort to characterize the viscous properties and the likelihood of future (and perhaps even past) planet formation in these disks. 11:50 to 12:10 J Bouwman ([Max-Planck-Institute, Heidelberg])Observational evidence for grain growthSession: 1 - Observations of Protoplanetary Discs The disks in Herbig Ae/Be and T Tauri systems are believed to be the birth sites of planetary systems. These disks are known to dissipate in about 10Myr, after which giant planet formation will be terminated. In this review I will discuss observational evidence for the onset of planet formation:the growth of sub-micron sized dust grains, typical for the ISM, into mm sized dust grains. To correctly interpret these observations, comparisons to experimental and theoretical studies elucidating the processes (growth, evaporation, condensation, crystallisation, and large scale mixing) acting on dust in protoplanetary disks, are required. This review will, therefore, extensively discuss the interplay between observations and experiments/theory. 12:10 to 12:40 Discussion (session chair: Jim Pringle)Session: 1 - Observations of Protoplanetary Discs 12:40 to 13:30 Lunch at Wolfson Court and posters 14:00 to 14:40 C Dominik ([Amsterdam])Review - models of protoplanetary disksSession: 2 - Protoplanetary Disc Modelling In my talk I will address a variety of modeling approaches to protoplanetary disks. I will discuss radiative transfer models that are used to derive spectral energy distributions and address the issues related to various geometrical structures in such disks and the pitfall of modeling these with codes not appropriate for complex geometries. I will discuss the latest models of the inner boundary of protoplanetary disks near the dust evaporation zone and show that a detailed treatment of the evaporation physics leads to interesting structure, size and chemical sorting, and possibly to instabilities as a source for observational variability, both in SED features and in interferometric observations. I will also discuss the latest suite of models covering dust settling and coagulation on a global scale in disks. Hydrodynamic and magnetohyrdodynamic models are beyond the scope of this review talk. 14:40 to 15:00 N Calvet ([Michigan])Recent results on the interpretation of observations of protoplanetary disksSession: 2 - Protoplanetary Disc Modelling I will show recent results on the interpretation of SEDs and spectra of protoplanetary disks around low mass stars. I will talk about recent Spitzer/IRS observations that indicate that disks are very settled even in extremely young populations. I will then talk about Spitzer/IRAS observations showing that the inner disks get increasingly settled as the population ages in primordial disks. I will show UV observations of molecular H that indicate that the gas in the inner disk disappears when the stars stop accreting, even if some dust and probably gas is left in the outer disks. I will talk about the transitional and pre-transitional disks, that is, disks with inner clearing and gaps, and speculate that they are possible phases for the final clearing of the inner disks. 15:00 to 15:30 Tea and posters INI 1 15:30 to 15:50 G Lesur ([Cambridge])Turbulent convection in accretion discsSession: 2 - Protoplanetary Disc Modelling Transport of angular momentum has always been a central problem of accretion disc theory. Since the discovery of the magnetorotational instability in accretion discs by Balbus and Hawley (1991), MRI-driven turbulence is believed to be the best candidate to explain anomalous transport in discs. Despite this result, several other routes to turbulence have been considered over the last two decades, with limited success. A possible alternative to MRI turbulence is turbulent convection, driven by an unstable vertical entropy gradient in the disc. Several studies have shown that convection was actually transporting angular momentum inward, and is therefore not favourable to accretion. In this presentation, I will revisit the problem of turbulent convection in accretion discs, using modern numerical methods. In particular, I will show that this hydrodynamic process could actually drive outward angular momentum transport if certain conditions are met, with an efficiency compatible with protoplanetary discs observations. 15:50 to 16:10 T Sano ([Osaka])Dead zones in protoplanetary disksSession: 2 - Protoplanetary Disc Modelling MHD turbulence driven by the magnetoroational instability (MRI) is the most promising mechanism of angular momentum transport in accretion disks. However protoplanetary disks are dense and cold so that the ionization fraction is extremely low. It is known that there must be dead zones in protoplanetary disks where the growth of MRI is suppressed significantly due to non-ideal MHD effects. The size of dead zones are related to the characteristics of dust grains. The gas and dust evolutions, or planet formation, are affected by the existence of the dead zones. The roles of the dead zones in planet formation scenario are summarized in this talk. 16:10 to 16:30 C Gammie ([Illinois])Self-gravitating disc evolutionSession: 2 - Protoplanetary Disc Modelling I will briefly review recent advances in modeling self-gravitating disc evolution, as well as some unsolved problems, particularly the long-term interaction of density waves with other forms of angular momentum transport such as MHD turbulence. 16:30 to 17:00 C Clarke ([Cambridge])The role of photoevaporation in disc dispersalSession: 2 - Protoplanetary Disc Modelling I first recapitulate former work explaining how the interplay between viscous evolution and extreme ultraviolet (EUV) photoevaporation produces a characteristic pattern of disc clearing, which invoves first rapid viscous draining of the inner disc (within a few A.U.) followed by rapid photoevaporation of the outer disc. This behaviour sets in at late times when the accretion rate through the disc is very low ($\sim 10^{10} M_\odot$ yr$^{-1}$). I then describe recent work which demonstrates that, contrary to previous estimates, Xray photoevaporation is in fact likely to be a major disc dispersal agent. The sequence of disc clearing phases is qualitatively similar to that described above but with two key differences: i) the photoevaporation rate is ten times higher and thus this clearing sets in earlier, when the disc accretion rate is $\sim 10^{-9} M_\odot$ yr$^{-1}$ and ii) a combination of the greater penetrating power of Xrays and the somewhat lower temperatures attained by Xray heated gas compared with the EUV case means that the peak wind mass loss occurs at $\sim 20$ A.U.. The size of the inner hole is thus $\sim 4$ times larger than in EUV photoevaporative models. We discuss the implications of this new result for models of disc clearing and the production of transition discs. 17:00 to 17:30 Discussion (session chair: Steve Balbus)Session: 2 - Protoplanetary Disc Modelling 17:30 to 18:30 Welcome Wine Reception INI 1 18:45 to 19:30 Dinner at Wolfson Court (Residents Only)