PROTOSTARS & PLANETS VI

Heidelberg, July 15-20, 2013

Program and Abstract Book(For handheld devices)

[Conference center map]

[Program]

[Posters]

[Participant list]

Organizers:Henrik Beuther (MPIA), Ralf Klessen (Uni-HD), Cornelis Dullemond (Uni-HD) andThomas Henning (MPIA)

Scientific Organizing Committee:Philippe André (CEA/SAp Saclay), JavierBallesteros-Paredes (UNAM), IsabelleBaraffe (Univ. of Exeter), Alan Boss (CarnegieInst.), John Bradley (LLNL), Nuria Calvet(Univ. of Michigan), Gael Chauvin (IPAG),Therese Encrenaz (Obs. de Paris), GuidoGaray (Univ. de Chile), Tristan Guillot (Obs.de la Côte d’Azur), Nader Haghighipour (IfA),Shigeru Ida (Tokyo Inst. of Technology), RayJayawardhana (Toronto), Willy Kley (Univ. ofTübingen), Alexander Krot (IfA), KatharinaLodders (Washington Univ. in St. Louis),Karl Menten (MPIfR), Michael Meyer (ETH),Alessandro Morbidelli (Obs. de la Côted’Azur), Ralph Pudritz (McMaster Univ.), BoReipurth (IfA), Dimitar Sasselov (CfA), Mo-tohide Tamura (NAOJ), Ewine van Dishoeck(Leiden Obs./MPE), Stephane Udry (Univ. ofGeneva), Alycia Weinberger (Carnegie Inst.)

This conference is sponsored by:

German Science Foundation

DFG Priority Program

“Physics of the Interstellar Medium”

DFG Collaborative Research Center

“The Milky Way System”

Max Planck Institute for Astronomy Heidelberg University

Center for Astronomy Heidelberg European Space Agency

http://www.dfg.dehttp://www.ism-spp.dehttp://www.zah.uni-heidelberg.de/sfb881/http://www.mpia.dehttp://www.uni-heidelberg.dehttp://www.zah.uni-heidelberg.dehttp://www.esa.int

Heidelberg Convention Center (“Stadthalle”)Neckarstaden 24, 69117 Heidelberg

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Review Talks

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Monday Tuesday Wednesday Thursday Friday Saturday

Registration

Welcome

Formation of Molecular Clouds

Mark Krumholz

Filaments to CoresPhilippe André

Origin of the IMFPaul Clark

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Star Formation RateChristoph Federrath

Magnetic Fields in SFHuabai Li

POSTER SESSION 1

Milky Way as SF EngineJohn Bally

COFFEE

RECEPTION ATTHE CASTLE

(drinks and fingerfood)

Massive Star FormationChris McKee

Disk FormationZhi-Yun Li

COFFEE

YSOs: Spitzer & HerschelAmy Stutz

Ages of Young StarsRob Jeffries

Star Clusters & FeedbackMatthew Bate

Multiplicity in Stellar EvolutionCathie Clarke

POSTER SESSION 1

COFFEE

Young Massive ClustersSteven Longmore

Public Talk onPlanet Formation

(in German)Willy Benz

Press Conference(in German)

Structure of PP DisksDmitry Semenov

Dust Evolution in PP Disks

Leonardo Testi

Volatiles in PP DisksColette Salyk

Water: From Clouds to PlanetsTed Bergin

Episodic AccretionJoel Green

Transport Processes in PP DisksGeoffroy Lesur

Stellar RotationSean Matt

Poster Prize Talk 1

CONFERENCE DINNERAT THE MOLKENKUR

(buses will be availablefor transport to theMolkenkur)

Jets and OutflowsSylvie Cabrit

Dispersal of PP DisksIlaria Pascucci

Transition DisksJames Muzerolle

Debris DisksBrenda Matthews

Planetesimal FormationAnders Johansen

Thermal Evolution of PlanetesimalsMario Trieloff

POSTER SESSION 2 POSTER SESSION 2

Terrestrial Planet FormationSean Raymond

Brown Dwarfs vs. Giant Planets

Gilles Chabrier

Giant PlanetsRavit Helled

Planet-Disk InteractionAurelien Crida

Planet Population SynthesisShigeru Ida

ExoplanetsDebra Fischer

Meteoritical ConstraintsThomas Stephan

Planetary Internal Structure

Jonathan Fortney

Exoplanetary AtmospheresNikku Madhusudhan

Long-term Planetary DynamicsMelvyn Davies

Astronomical Conditions for Life

Manuel Guedel

Deuterium FractionationPaola Caselli

Poster Prize Talk 2

Final Word

BOAT TOURCOFFEE COFFEE COFFEE

COFFEE COFFEE COFFEE COFFEE

Sunday

Registration&

“Pre-conferenceget-together”

Location: Convention Center (“Stadthalle”)

(drinks available)

Monday, July 15

8:30 REGISTRATION9:45 Welcome & Organisatorial Info

Session 1 ”Molecular Clouds and StarFormation I” Bo Reipurth

10:15 Dobbs,Krumholzet al.

Formation of molecu-lar clouds and globalconditions for star for-mation [abs]

11:00 Andr é,Di Frances-co et al.

From filamentarynetworks to densecores in molecularclouds: Toward anew paradigm for starformation [abs]

11:45 Offner,Clark et al.

The origin and uni-versality of the ini-tial mass function

[abs]12:30 LUNCH BREAK

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Monday, July 15

Session 2 ”Molecular Clouds and StarFormation II” Philippe Andr é

14:30 Padoan,Federrath ,et al.

The star formation rateof molecular clouds

[abs]15:15 Li , et al. The link between

magnetic fields andcloud/star formation

[abs]16:00 COFFEE BREAK16:30 – Poster Session 1 –17:45 Molinari,

Bally ,et al.

The Milky Way as astar formation engine

[abs]18:30 (walk to the castle)19:00 RECEPTION AT THE CASTLE

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Tuesday, July 16

Session 3 ”Molecular Clouds and StarFormation III” Ewine van Dishoeck

8:30 Tan,McKee ,et al.

Massive star formation[abs]

9:15 Li , et al. The earliest stages ofstar and planet forma-tion: Core collapse,and the formation ofdisks and outflows

[abs]10:00 COFFEE BREAK11:00 Dunham,

Stutz ,et al.

The evolution of pro-tostars: Insights fromten years of infraredsurveys with SPITZERand HERSCHEL [abs]

11:45 Soderblom,Jeffries ,et al.

Ages of young stars[abs]

12:30 LUNCH BREAK

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Tuesday, July 16

Session 4 ”Molecular Clouds and StarFormation IV” Ralph Pudritz

14:30 Krumholz,Bate , et al.

Star cluster formationand feedback [abs]

15:15 Reipurth,Clarke ,et al.

Multiplicity in earlystellar evolution [abs]

16:00 COFFEE BREAK16:30 – Poster Session 1 –17:45 Longmore ,

et al.The formation andearly evolution ofyoung massive clus-ters [abs]

20:00 Public Talk (in German) byWilly Benz at the Old Auditorium

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Wednesday, July 17

Session 5 ”Disk Formation and Evolution I”Michael Meyer

8:30 Dutrey,Semenov ,et al.

Physical and chemi-cal structure of planet-forming disks probedby millimeter obser-vations and modelling

[abs]9:15 Testi , et al. Dust evolution in pro-

toplanetary disks [abs]10:00 COFFEE BREAK11:00 Pontoppidan,

Salyk ,et al.

Volatiles in protoplane-tary disks [abs]

11:45 v. Dishoeck,Bergin ,et al.

Water: From clouds toplanets [abs]

12:30 LUNCH BREAK

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Wednesday, July 17

Session 6 ”Disk Formation and Evolution II”Shigeru Ida

14:30 Audard,Green ,et al.

Episodic accretion inyoung stars [abs]

15:15 Turner,Lesur ,et al.

Transport and accre-tion in planet-formingdisks [abs]

16:00 COFFEE BREAK16:30 Bouvier,

Matt , et al.Angular momentumevolution of younglow-mass stars andbrown dwarfs: Ob-servations and theory

[abs]17:15 Talk by Poster Prize Winner 118:45 (buses depart to Molkenkur)19:00 CONFERENCE DINNER

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Thursday, July 18

Session 7 ”Disk Formation and Evolution III”Motohide Tamura

8:30 Frank,Cabrit ,et al.

Jets and outflows fromstar to cloud: Obser-vations confront theory

[abs]9:15 Alexander,

Pascucci ,et al.

The dispersal of proto-planetary discs [abs]

10:00 COFFEE BREAK11:00 Espaillat,

Muzerolle ,et al.

An observational per-spective of transitionaldisks around T Tauristars [abs]

11:45 Matthews ,et al.

Observations, Model-ing and Theory of De-bris Discs [abs]

12:30 LUNCH BREAK

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Thursday, July 18

Session 8 ”Planets: Search, Formationand Evolution I” Willy Kley

14:30 Johansen ,et al.

The multifaceted plan-etesimal formationprocess [abs]

15:15 Gail,Trieloffet al.

Early thermal evolu-tion of planetesimalsand its impact onprocessing and datingof meteoritic material

[abs]16:00 COFFEE BREAK16:30 – Poster Session 2 –17:45 Raymond ,

et al.Terrestrial planet for-mation at home andabroad [abs]

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Friday, July 19

Session 9 ”Planets: Search, Formationand Evolution II” Isabelle Baraffe

8:30 Chabrier ,et al.

Formation of browndwarfs vs giant plan-ets: Confronting the-ory with observations

[abs]9:15 Helled ,

et al.Giant planet forma-tion, evolution, andinternal structure

[abs]10:00 COFFEE BREAK11:00 Baruteau,

Crida ,et al.

Planet-disc inter-actions and earlyevolution of planetarysystems [abs]

11:45 Benz, Ida,et al.

Planet population syn-thesis [abs]

12:30 LUNCH BREAK

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Friday, July 19

Session 10 ”Planets: Search, Formationan Evolution III” Alessandro Morbidelli

14:30 Fischer ,et al.

New exoplanetary sys-tems [abs]

15:15 Madhusud-han , et al.

Exoplanetary Atmo-spheres [abs]

16:00 COFFEE BREAK16:30 – Poster Session 2 –17:45 Baraffe,

Fortney ,et al.

Planetary internalstructures [abs]

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Saturday, July 20

Session 11 ”Planets: Search, Formationand Evolution IV” Nader Haghighipour

8:30 Davies ,et al.

The long-term dy-namical evolution ofplanetary systems

[abs]9:15 Davis,

Stephanet al.

Samples of the solarsystem: recent devel-opments [abs]

10:00 COFFEE BREAK11:00 Ceccarelli,

Caselli ,et al.

Deuterium fractiona-tion: The ariane threadfrom the pre-collapsephase to meteoritesand comets [abs]

11:45 Talk by Poster Prize Winner 212:00 Güdel ,

et al.Astrophysical con-ditions for planetaryhabitability [abs]

12:45 Final word – End of conference

14:30 BOAT TOUR

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Abstracts of the Review Talks

FORMATION OF MOLECULAR CLOUDSAND GLOBAL CONDITIONS FOR STARFORMATION [prog]C. Dobbs, M. Krumholz, J. Ballesteros-Paredes, A. Bolatto, Y. Fukui, M. Heyer, M.Mac Low, E. Ostriker, E. Vazquez-Semadeni

Giant molecular clouds (GMCs) are the primary reser-voirs of cold, star-forming molecular gas in the MilkyWay and similar galaxies, and thus any understandingof star formation must encompass a model for GMC for-mation, evolution, and destruction. These models arenecessarily constrained by measurements of interstel-lar molecular and atomic gas, and the emergent, new-born stars. Both observations and theory have under-gone great advances in recent years, the latter drivenlargely by improved numerical simulations, and the for-mer by the advent of large-scale surveys with new tele-scopes and instruments. This chapter reviews the cur-rent state of the field.

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FROM FILAMENTARY NETWORKS TODENSE CORES IN MOLECULAR CLOUDS:TOWARD A NEW PARADIGM FOR STARFORMATION [prog]P. André, J. Di Francesco, S.-I. Inutsuka, R.Pudritz, D. Ward-Thompson, J. Pineda

We review recent progress in our understanding of thephysics controlling the earliest evolutionary phases ofstar formation. Since PPV seven years ago, one areathat has seen the most dramatic advances has beenthe characterization of the link between star formationand the structure of the cold interstellar medium (ISM).In particular, extensive studies of the nearest star-forming clouds of our Galaxy with the Herschel SpaceObservatory have provided us with unprecedented im-ages of the initial and boundary conditions of the starformation process. The Herschel images reveal an in-tricate network of filamentary structures in every inter-stellar cloud. The observed filaments share commonproperties such as their central widths - but only thedensest ones contain prestellar cores, the seeds of fu-ture stars. Overall, the Herschel submillimeter data, aswell as other observations from, e.g., near-IR extinctionstudies, favor a scenario in which interstellar filamentsand prestellar cores represent two key steps in the starformation process: first supersonic turbulence stirs upthe gas, giving rise to a universal web-like structure in

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the ISM, then gravity takes over and controls the furtherfragmentation of filaments into prestellar cores and ulti-mately protostars.

The new observational results connect remark-ably well with nearly a decades worth of numerical sim-ulations and theory which have consistently shown thatthe ISM should be highly filamentary on all scales andthat star formation is intimately connected with self-gravitating filaments.

We thus attempt to synthesize a comprehen-sive physical picture that arises from the confrontationof recent observations and simulations. We also em-phasize how the apparent complexity of cloud structureand star formation may be governed by relatively sim-ple universal processes - from filamentary clumps togalactic scales.

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THE ORIGIN AND UNIVERSALITY OF THEINITIAL MASS FUNCTION [prog]S. Offner, P. Clark, P. Hennebelle, N. Bastian,M. Bate, P. Hopkins, E. Moraux, A. Whitworth

We review current theories for the origin of the Stel-lar Initial Mass Function (IMF) with particular focus onthe extent to which the IMF can be considered univer-sal across various environments. To place the issuein an observational context, we summarize the tech-niques used to determine the IMF for different stellarpopulations, the uncertainties affecting the results, andthe evidence for systematic departures from universal-ity under extreme circumstances. We next considertheories for the formation of prestellar cores by turbu-lent fragmentation and the possible impact of variousthermal, hydrodynamic and magneto-hydrodynamic in-stabilities. We address the conversion of prestellarcores into stars, and evaluate the roles played by differ-ent processes: competitive accretion, dynamical frag-mentation, ejection and starvation, filament fragmen-tation and filamentary accretion flows, disc formationand fragmentation, critical scales imposed by thermo-dynamics, and magnetic braking. We present expla-nations for the characteristic shapes of the Present-Day Prestellar Core Mass Function and the IMF andconsider what significance can be attached to their ap-parent similarity. Substantial computational advances

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have occurred in recent years, and we review the nu-merical simulations that have been performed to predictthe IMF directly and discuss the influence of dynamics,time-dependent phenomena, and initial conditions.

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THE STAR FORMATION RATE OF MOLEC-ULAR CLOUDS [prog]P. Padoan, C. Federrath, G. Chabrier, N.Evans, D. Johnstone, J. Jørgensen, C. Mc-Kee, Å. Nordlund

We review recent advances in the analytical and nu-merical modeling of the star formation rate in molecu-lar clouds and discuss the available observational con-straints. We focus on molecular clouds as the funda-mental star formation sites, rather than on the larger-scale processes that form the clouds and set their prop-erties. Molecular clouds are shaped into a complex fil-amentary structure by supersonic turbulence, with onlya small fraction of the cloud mass channeled into col-lapsing protostars over a free-fall time of the system.In recent years, the physics of supersonic turbulencehas been widely explored with computer simulations,leading to statistical models of this fragmentation pro-cess, and to the prediction of the star formation rateas a function of fundamental physical parameters ofmolecular clouds, such as the virial parameter, the rmsMach number, the compressive fraction of the turbu-lence forcing, and the ratio of magnetic to gas pressure.Infrared space telescopes, as well as ground-based ob-servatories have provided unprecedented probes of thefilamentary structure of molecular clouds and the loca-tion of forming stars within them. We may thus be on

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the verge of a breakthrough in our understanding of starformation, and particularly of the star formation rate ofmolecular clouds.

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THE LINK BETWEEN MAGNETICFIELDS AND CLOUD/STAR FORMATION

[prog]H.-B. Li, A. Goodman, M. Houde, Z.-Y. Li, G.Novak, T. Sridharan

The question of whether magnetic fields play an impor-tant role in the processes of molecular cloud and starformation has been debated for decades. Recent ob-servations reveal a simple picture that may help illumi-nate these questions: magnetic fields have a tendencyto preserve their orientation at all scales that have beenprobed - from 100-pc scale inter-cloud media down tosub-pc scale cloud cores. This ordered morphologyhas implications for the way in which self-gravity andturbulence should interact with magnetic fields: bothgravitational contraction and turbulent velocities shouldbe anisotropic, due to the influence of dynamically im-portant fields. Such anisotropy is largely observed.Here we review these recent observations and discusshow they can improve our understanding of cloud/starformation.

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THE MILKY WAY AS A STAR FORMATIONENGINE [prog]S. Molinari, J. Bally, J.-P. Bernard, S. Glover,P. Martin, T. Moore, A. Noriega-Crespo, R.Plume, L. Testi, E. Vazquez-Semadeni, A.Zavagno

We review and discuss the latest observational sce-nario globally emerging from the latest generation ofcontinuum and spectroscopic global-scale surveys ofthe mid-plane of the Galaxy from infrared to radio wave-lengths, in terms of cloud formation and evolution, starand clump formation rate and efficiency throughout theGalaxy, evidence for density thresholds for the forma-tion of protocluster-forming clumps, as well as the roleof large-scale filamentary structures in channeling dif-fuse ISM into gravitationally bound clumps. The newview of the Milky Way thus assembled will be discussedin the context of competing theoretical frameworks dis-tinguishing between ”slow” and ”fast” formation, outlin-ing some of the challenges that this body of evidenceposes to a variety of theoretical scenarios for large-scale star formation.

We will review the most recent methods andevolutionary indicators used to classify the star forma-tion activity in molecular clumps, comparing the dif-ferent possible derivations of the local SFR and dis-cussing its variation as a function of Galactocentric ra-

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dius. The order-of-magnitude increase in the number ofsources (mostly clumps) that are revealed in state-of-the-art infrared and submillimeter Galaxy-wide surveysmake such studies possible with an unprecedented sta-tistical significance.

We will also review the present status of ourunderstanding of the Galaxy as a global star formationengine in the context of similar studies in extragalacticsystems, evaluating how the data on our own Galaxycompare with the proposed global star formation lawsthat relate properties of the interstellar medium to thestar formation rate.

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MASSIVE STAR FORMATION [prog]J. Tan, M. Beltran, P. Caselli, F. Fontani, A.Fuente, M. Krumholz, C. McKee, A. Stolte

The enormous radiative and mechanical luminosities ofmassive stars impact a vast range of scales and pro-cesses, from the reionization of the universe, to theevolution of galaxies, to the regulation of the interstellarmedium, to the formation of star clusters, and even tothe formation of planets around stars in such clusters.Furthermore, the synthesis and dispersal of heavy ele-ments by massive stars plays a key role in the chemi-cal evolution of the cosmos. Achieving a rigorous theo-retical understanding of massive star formation is thusan important goal of contemporary astrophysics. Thiseffort can also be viewed as a major component ofthe development of a general theory of star formationthat seeks to explain the birth of stars of all massesand from all the variety of star-forming environments.Two main classes of theories for massive star forma-tion are under active study, “Core Accretion” and “Com-petitive Accretion”. In Core Accretion, the initial con-ditions of star formation are self-gravitating, centrallyconcentrated cores that condense from the surround-ing, fragmenting clump environment with a range ofmasses. They then undergo relatively ordered collapsevia a central disk to form a single star or a small-N mul-tiple. In this case, the pre-stellar core mass function

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has a similar form to the stellar initial mass function. InCompetitive Accretion, the material that forms a mas-sive star is drawn more chaotically from a wider regionof the clump without passing through a phase of beingin a massive, coherent core. In this case, massive starformation must proceed hand in hand with star clusterformation. If stellar densities become very high nearthe cluster center, then collisions between stars couldalso be involved in forming the most massive stars. Wereview recent theoretical and observational progress to-wards understanding massive star formation, consider-ing a range of observed galactic star-forming environ-ments, physical and chemical processes, comparisonswith low and intermediate-mass stars, and connectionsto star cluster formation.

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THE EARLIEST STAGES OF STAR ANDPLANET FORMATION: CORE COLLAPSE,AND THE FORMATION OF DISKS ANDOUTFLOWS [prog]Z.-Y. Li, R. Banerjee, R. Pudritz, J. Joer-gensen, H. Shang, R. Krasnopolsky, A. Maury

The formation of stars and planets are connectedthrough disks. Our theoretical understanding of diskformation has undergone drastic changes since PPV,and we are on the brink of an ALMA-enabled revolutionin disk observation. Disk formation - once thought tobe a trivial consequence of the conservation of angu-lar momentum - is far more subtle in magnetized gas.In this case, the rotation can be strongly magneticallybraked. Indeed, both analytic arguments and numeri-cal simulations have shown that disk formation is sup-pressed in the strict ideal MHD limit for the observedlevel of core magnetization, at least for idealized, lam-inar, axisymmetric cores with ordered magnetic fields.In the theoretical literature, this “catastrophic” magneticbraking characterizes the situation wherein the angu-lar momentum of an idealized collapsing core is nearlycompletely removed by magnetic braking close to thecentral object. We will review what is known about this“magnetic braking catastrophe”, possible ways to re-solve it, and the current status of early disk observa-tions. Possible resolutions include non-ideal MHD ef-

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fects (ambipolar diffusion, Ohmic dissipation and Halleffect), magnetic interchange instability in the inner partof protostellar accretion flow, turbulence, misalignmentbetween the magnetic field and rotation axis, and de-pletion of the slowly rotating envelope by outflow strip-ping or accretion. We will assess the pros and cons ofeach of these proposed resolutions and put them intoan over-arching physical context. Outflows are also inti-mately linked to disk formation; they are a natural prod-uct of magnetic fields and rotation and are importantsignposts of star formation. We review new develop-ments on early outflow generation since PPV. The prop-erties of early disks and outflows are a key componentof planet formation in its early stages and we will reviewthese major connections.

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THE EVOLUTION OF PROTOSTARS: IN-SIGHTS FROM TEN YEARS OF INFRAREDSURVEYS WITH SPITZER AND HERSCHEL[prog]M. Dunham, A. Stutz, L. Allen, N. Evans, W.Fischer, S.T. Megeath, P. Myers, S. Offner, C.Poteet, J. Tobin, E. Vorobyov

Stars and planets form from the gravitational collapse ofdense molecular cloud cores. The protostellar phase isthe period during which mass accretes from the core,through an accretion disk formed by conservation ofangular momentum, and onto a hydrostatically sup-ported protostar. It is the phase during which the ini-tial masses of stars and the initial conditions for planetformation are set, thus understanding how protostarsevolve is a crucial ingredient for developing a generalunderstanding of star and planet formation. Identifica-tion and characterization of protostars has traditionallybeen hindered by the embedded nature of these ob-jects. Over the past ten years, new observational ca-pabilities provided by the Spitzer Space Telescope andHerschel Space Observatory have enabled wide-fieldinfrared surveys of entire star-forming clouds with highsensitivities, leading to remarkable progress in our un-derstanding of protostellar evolution. We review severalkey advances in the field over the past decade, focus-

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ing both on the observations themselves and the con-straints these large-area surveys are placing on theo-retical models of star formation and protostellar evolu-tion. We also emphasize several open questions anddebates and outline the future observational and theo-retical work necessary to further advance the field.

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AGES OF YOUNG STARS [prog]D. Soderblom, L. Hillenbrand, R. Jeffries, E.Mamajek, T. Naylor

Determining the sequence of events in the formationof stars and planetary systems and their time-scales isessential for understanding these processes, yet estab-lishing ages is fundamentally difficult because we lackdirect indicators. In this review we discuss the problemof ages for young stars, specifically for those less than∼ 100 Myr old.

We start by establishing a reliable scale scalefor young stars using the measurement of the LithiumDepletion Boundary (LDB) in young clusters, a methodthat involves fairly simple and well-established physicsand observations. We show that LDB ages are consis-tent with those from the upper main sequence and themain sequence turn-off if modest core convection is in-cluded in the models of higher-mass stars. The LDBmethod can be used to set limits on the age of individ-ual objects but is primarily applicable to groups of stars.

We then review the available methods for ageestimation, which include kinematic traceback of younggroups, placing stars in HRDs, pulsations and seismol-ogy, gravity differences, rotation, activity, and lithiumabundance as age indicators. We list the knownstrengths and weaknesses of each of these. Some ofthese techniques are useful within certain limits (such

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as age and mass ranges) and others are entirely prob-lematic.

We look at the issue of age spreads within star-forming regions and how well they can be quantified.Finally, we offer suggestions and recommendations toguide interpretation of observations, and we show howthe current situation can be improved over the next fewyears.

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STAR CLUSTER FORMATION AND FEED-BACK [prog]M. Krumholz, M. Bate, H. Arce, J. Dale, R.Gutermuth, R. Klein, Z.-Y. Li, F. Nakamura, Q.Zhang

Stars do not generally form in isolation. Instead, theyform in clusters, and in these clustered environmentsnewborn stars can have profound effects on one an-other and on their parent gas clouds. Feedback fromclustered stars is almost certainly responsible for anumber of otherwise puzzling facts about star forma-tion: that it is an inefficient process that proceeds slowlywhen averaged over galactic scales; that it producesmostly unbound field stars rather than bound clusters;and that it produces an IMF with a distinct peak in therange 0.1 − 1 Msun, rather than an IMF dominated bybrown dwarfs. In this review we summarize current ob-servational constraints and theoretical models for thecomplex interplay between clustered star formation andfeedback.

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MULTIPLICITY IN EARLY STELLAR EVO-LUTION [prog]B. Reipurth, A.P. Boss, C.J. Clarke, S.P.Goodwin, L.F. Rodriguez, K.G. Stassun, A.Tokovinin, H. Zinnecker

Observations from optical to centimeter wavelengthshave demonstrated that multiple systems of two ormore bodies is the norm at all stellar evolutionarystages. Multiple systems are widely agreed to resultfrom the collapse and fragmentation of cloud cores, de-spite the inhibiting influence of magnetic fields. Surveysof Class 0 protostars with mm interferometers have re-vealed a very high multiplicity frequency of about 2/3,even though there are observational difficulties in re-solving close protobinaries, thus supporting the possi-bility that all stars could be born in multiple systems.Near-infrared adaptive optics observations of Class Iprotostars show a lower binary frequency relative tothe Class 0 phase, a declining trend that continuesthrough the Class II/III stages to the field population.This loss of companions is a natural consequence ofdynamical interplay in small multiple systems, leadingto ejection of members. We discuss observational con-sequences of this dynamical evolution, and its influ-ence on circumstellar disks, and we review the evo-lution of circumbinary disks and their role in definingbinary mass ratios. Special attention is paid to eclips-

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ing PMS binaries, which allow for observational testsof evolutionary models of early stellar evolution. Manystars are born in clusters and small groups, and wediscuss how interactions in dense stellar environmentscan significantly alter the distribution of binary separa-tions through dissolution of wider binaries. The bina-ries and multiples we find in the field are the survivorsof these various destructive processes, and we providea detailed overview of the multiplicity statistics of thefield, which form a boundary condition for all modelsof binary evolution. Finally we discuss various forma-tion mechanisms for massive binaries, and the origin ofmassive trapezia and their role in the dynamical evolu-tion of clusters.

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THE FORMATION AND EARLY EVOLU-TION OF YOUNG MASSIVE CLUSTERS

[prog]S. Longmore, J. Alves, J. Bally, N. Bastian, E.Bressert, J. Dale, D. Kruijssen, J. Rathborne,L. Testi, A. Stolte

We review the formation and early evolution of themost massive (and dense) young stellar clusters in ourGalaxy, and the role this can play in our understandingof star and planet formation as a whole. We start byreviewing the global properties and environmental con-ditions of the known young massive clusters (YMCs)and their progenitor gas clouds. We then focus on theobserved embedded dense core and (proto)stellar pop-ulations within these clusters, and discuss how suchlarge stellar systems can potentially simultaneously dis-tinguish between competing cluster formation modelsand provide the strongest constraints on the physicalorigin of the stellar initial mass function. After reviewingthe current theoretical framework for the formation andevolution of YMCs, we summarise the debate on twokey open questions: infant (im)mortality and the evi-dence for/against significant age spreads within YMCs.We then discuss which fraction of all stars and plan-ets, including our own solar system, may have formedin extreme environmental conditions (proximity to high-mass stars, high (proto)stellar den- sities etc) similar to

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those found in these clusters, rather than the more be-nign conditions found in local, low-mass star formationregions. Finally, we review how the most massive anddense young clusters can be used as a bridge linkingwhat we learn about star and planet formation in thenearest-by re- gions, to starburst systems in the LocalUniverse, globular cluster formation and star/planet for-mation at the earliest epochs of the universe.

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PHYSICAL AND CHEMICAL STRUCTUREOF PLANET-FORMING DISKS PROBEDBY MILLIMETER OBSERVATIONS ANDMODELLING [prog]A. Dutrey, D. Semenov, E. Chapillon, U.Gorti, F. Gueth, S. Guilloteau, F. Hersant, M.Hogerheijde, M. Hughes, H. Nomura, V. Pietu,C. Qi, V. Wakelam, G. Meeus

Protoplanetary disks composed of dust and gas areubiquitous around young stars. Their lifetime, appear-ance, and structure are determined by an interplaybetween stellar radiation, gravity, thermal pressure,magnetic field, gas viscosity, turbulence, and rotation.Molecules and dust serve as major heating and coolingagents in disks. Dust grains dominate the disk opaci-ties, reprocess most of the stellar radiation, and shieldmolecules from ionizing UV/X-ray photons. In turn, theratio of ions to neutral molecules determines the levelof turbulence and redistribution of the angular momen-tum. Therefore, the evolution of the gas and dust is akey element that regulates the efficiency and timescaleof planet formation. The situation is complicated by thefact that the dust and gas physically and chemically in-teract. The dust and gas are initially dynamically wellcoupled because of the very small sizes of the dustparticles, but later grains evolve differently because of

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significant growth in the disks, up to cm size and larger.Grain growth is more pronounced in very dense, innerdisk regions. After large dust grains become dynami-cally decoupled from the gas, they gravitationally set-tle towards the disk midplane, and spiral inwards veryfast or experience mutual collisions and get destroyed.Collisionally-generated small grains are either collectedby larger grains locally or swept up by turbulence intothe disk atmosphere. Dust settling and turbulent stirringradially and vertically change the dust-to-gas ratio andaverage dust sizes. All these processes affect the diskthermal and density structure, and, as such, control itschemical composition. In the dense disk midplane thethermal equilibrium between gas and dust is achieved,with dust transferring heat to gas by rapid gas-grain col-lisions. The disk midplane is well shielded from stellarradiation and thus is ”dark”, with low ionization degreeand low turbulence velocities. The outer disk midplaneis so cold that many molecules severely freeze out ontodust grains there, leading to the production of complexices. Above the midplane a more dilute region is lo-cated, where gas-grain collisional coupling is no longerefficient, and dust and gas temperatures start to departfrom each other, with the latter being usually hotter. Theupper surface disk layer is warmer than the midplanesince the heating photons that come from the star areabsorbed there by small dust grains or PAHs. This layeris more ionized and dynamically active, with rich gas-

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phase and gas-grain chemistry, leading to the synthesisof numerous gaseous species. Finally, in heavily irra-diated, ionized, hot and dilute atmosphere only simpleatoms, ions, photostable radicals and PAHs are able tosurvive.

The above picture is far more complicated asdisks dynamically evolve and build up planetary sys-tems, changing drastically disk gas and dust densitystructures. Detailed studies of protoplanetary disks re-main an observationally challenging task because disksare compact low-mass objects which appear opticallythick at visual and infrared wavelengths. One usesmillimeter/sub-millimeter observations to peer throughtheir structure. Since observations of the most domi-nant species in disks, H2, are impossible (except of thewarm upper layers via its weak quadrupole IR transi-tions), other molecules are employed to trace disk kine-matics, temperature, density, and chemical structure.Apart from a handful of molecules, like CO, HCO+, CS,CN and HCN, the molecular content of protoplanetarydisks remains largely unknown. The spatial distribu-tion of molecular abundances is still poorly determined,hampering a detailed comparison with existing chem-ical models. Due to the complexity of the molecularline excitation, unambiguous interpretation of the ob-servational results also necessitates advanced model-ing of the disk physical structure and evolution, chemi-cal history, and radiative transfer. Over the past decade

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significant progress has been achieved in our under-standing of disk chemical composition. Since PPV, ma-jor breakthroughs have been reached. Upgraded andnew mm/submm facilities (IRAM, SMA, Herschel andALMA) have permitted the detection of new molecu-lar species (DCN, H2O, HC3N...) at better spatial andfrequency resolution, while disk models have benefitedfrom improvements in astrochemistry databases (likeKIDA and UDFA’06), development of coupled thermo-chemical disk physical models, line radiative transfercodes, and better analysis tools.

This review will present and discuss the impactof such improvements on our understanding of the diskphysical structure and chemical composition.

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DUST EVOLUTION IN PROTOPLANETARYDISKS [prog]L. Testi, S. Andrews, T. Birnstiel, J. Blum, J.Carpenter, C. Dominik, A. Isella, A. Natta, L.Ricci, J. Williams, D. Wilner

In the core accretion scenario for the formation of plan-etary rocky cores, the first step toward planet formationis the growth of dust grains into larger and larger ag-gregates and eventually planetesimals. Although dustgrains are thought to grow from the submicron sizestypical of interstellar dust to micron size particles in thedense regions of molecular clouds and cores, it is atthe high densities reached on the protoplanetary disksmidplane that the growth from micron size particles topebbles and kilometre size bodies has to occur. Thisis a critical step for the formation of planetary systemsand the last stage of solids evolution that can be ob-served directly in young extrasolar systems before theappearance of large planetary-size bodies.

Tracing the properties of dust in the disk mid-plane, where the bulk of the material for planet for-mation resides, requires sensitive observations at longwavelengths (sub-mm through cm waves). At thesewavelengths, the measured dust opacity can be re-lated to the grain size distribution. In recent years theupgrade of the existing (sub-)mm arrays, the start ofALMA Early Science operations and the upgrade of the

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VLA have allowed a significant progress in our abilityto provide observational constraints to the models ofdust evolution in protoplanetary disks. Laboratory ex-periments and numerical simulations have allowed usto improve the understanding of the physical processesof grain-grain collisions, which are the foundation for themodels of dust evolution in disks.

In this chapter we cover the available con-straints on the physics of grain-grain collisions as theyemerge from laboratory experiments and numericalcomputations. We then review the status of our theo-retical understanding of the global processes governingthe evolution of solids in protoplanetary disks. We dis-cuss the results of dust settling and growth and the ra-dial transport of grains, as given by different dust evolu-tion models, from fractal to compact growth, and outlinethe predicted observable signatures of these effects.We summarize how the dust opacity depends on theproperties of the dust grains, as this is the property thatlinks the theoretical evolution models with observationalcharacteristics.

We discuss the recent developments in thestudy of grain growth in molecular cloud cores and incollapsing envelopes of protostars as these likely pro-vide the initial conditions for the dust in protoplanetarydisks. We then discuss the current observational evi-dence for the growth of grains in young protoplanetarydisks from millimeter surveys, as well as the very re-

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cent evidence of radial variations of the dust proper-ties in disks. We also include a brief discussion of theconstraints on the small end of the grain size distribu-tion and on dust settling as derived from optical, near-, and mid-IR observations. The observations are dis-cussed in the context of global dust evolution models,in particular we focus on the emerging evidence for avery efficient early growth of grains in disks and the ra-dial distribution of maximum grain sizes as the resultof growth barriers in disks. We will also highlight thelimits of the current models of dust evolution in disksincluding the need to slow the radial drift of grains toovercome the migration/fragmentation barrier. Recentresults from ALMA observations of grain growth in disksaround brown dwars and transitional disks are also in-cluded.

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VOLATILES IN PROTOPLANETARY DISKS[prog]K. Pontoppidan, C. Salyk, E. Bergin, S.Brittain, B. Marty, O. Mousis, K. Oberg

Volatiles are compounds with low sublimation temper-atures, and they make up most of the condensiblemass in typical planet-forming environments. They typ-ically consist of relatively small, often hydrogenated,molecules based on the abundant elements carbon,nitrogen and oxygen. Volatiles are central to the pro-cess of planet formation, forming the backbone of a richchemistry that sets the initial conditions for the forma-tion of planetary atmospheres, and acts as a solid massreservoir catalyzing the formation of planet and plan-etesimals. Since Protostars and Planets V, our under-standing of the evolution of volatiles in protoplanetaryenvironments has grown tremendously. This growthhas been driven by rapid advances in observations andmodels of protoplanetary disks, and of a deepening un-derstanding of the cosmochemistry of the solar system.Indeed, it is only in the past few years that represen-tative samples of molecules have been discovered ingreat abundance throughout protoplanetary disks (CO,H2O, HCN, C2H2, CO2, H2D+, HCO+) - enough to be-gin building a complete budget for the most abundantelements after hydrogen and helium. The spatial distri-butions of key volatiles are being mapped, snow lines

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are directly seen and quantified, and distinct chemicalregions within protoplanetary disks are being identified,characterized and modeled. Theoretical processes in-voked to explain the solar system record are now be-ing observationally constrained in protoplanetary disks,including transport of icy bodies and concentration ofbulk condensibles, strong thermal and chemical pro-cessing of inner disk material, along with the chemicallygentle accretion of pristine material from the interstellarmedium in the outer disk. This chapter focuses on mak-ing the first steps toward knowing whether the planetformation processes driving the final chemical makeupof our solar system are universal.

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WATER: FROM CLOUDS TO PLANETS[prog]E. van Dishoeck, E. Bergin, D. Lis, J. Lunine

Water is key molecule in the chemistry and physicsof protostellar and (proto)planetary environments andis associated with the emergence of life on Earth andlikely on planets elsewhere in the universe. Investiga-tions of interstellar water have been complicated, how-ever, by the fact that thermal water vapor emission canonly be observed from space platforms. Thanks to anumber of recent space missions, culminating with theHerschel Space Observatory, an enormous step for-ward has been made in our understanding of wherewater is formed in space, what its abundance is in var-ious physical environments, and how it is transportedfrom collapsing clouds to forming planetary systems.At the same time, new results are emerging on water inour own Solar system and in the atmospheres of exo-planets. This talk will attempt to tie together the latestinformation on water from the different subfields of ’Pro-tostars & Planets’ into a coherent story of the water trailfrom clouds to planets. Recent results will be summa-rized and open questions highlighted.

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EPISODIC ACCRETION IN YOUNG STARS[prog]M. Audard, P. Abraham, M. Dunham, J.Green, N. Grosso, K. Hamaguchi, J. Kastner,A. Kospal, G. Lodato, M. Romanova, S.Skinner, E. Vorobyov, Z. Zhu

Since the last major review in Protostars and PlanetsIV, the topic of episodic accretion has gained signifi-cant interest in the star formation community. It is nowviewed as a common, though still poorly understood,phenomenon in low-mass star formation. The FU Ori-onis objects (FUor) are long-studied examples of thisphenomenon. FUors are believed to undergo accre-tion outbursts during which the accretion rate rapidly in-creases from typically 10−7 M⊙/yr to 10−4 M⊙/yr, andremains elevated over timescales of several decadesor more. EXors, a loosely defined class of pre-main se-quence stars, exhibit similar but shorter and repetitiveoutbursts, associated with lower accretion rates. Therelationship between the two classes, and their relation-ship to the standard pre-main sequence evolutionarysequence, is an open question: do they form two dis-tinct classes, are they triggered by the same physicalmechanism, and do they occur in the same evolution-ary phases? Over the past couple of decades, manytheoretical and numerical models have been developedto explain the origin of FUor and EXor outbursts. In

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parallel, such accretion bursts have been detected atincreasing rate, and each individual outburst is morecarefully scrutinized and monitored across the electro-magnetic spectrum. These rapid advances have ledour team of observers and theorists to review our con-temporary understanding of episodic accretion from thetheoretical, numerical, and observational points of view,and to highlight the most promising directions for thisfield of star formation in the near- and long-term. Wesummarize key observations of pre-main sequence staroutbursts across the electromagnetic spectrum, and re-view the latest thinking on outburst triggering mecha-nisms, the propagation of outbursts from star/disk todisk/jet systems, the relationships between classicalEXors and FUors, and newly discovered outburstingsources – all of which shed new light on episodic ac-cretion.

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TRANSPORT AND ACCRETION INPLANET-FORMING DISKS [prog]N. Turner, S. Fromang, C. Gammie, H. Klahr,G. Lesur, M. Wardle, X. Bai

Planets appear to form in environments shaped bythe gas flowing through protostellar disks to the cen-tral young stars. The flows in turn are governed bythe transfer of orbital angular momentum. Here wesummarize current understanding of the transfer pro-cesses best able to account for the flows, includingmagneto-rotational turbulence, magnetically-launchedwinds, vortices driven by hydrodynamical instabilities,and self-gravitational instability. For each process inturn we outline the major achievements of the pastfew years and the outstanding questions remaining.We underscore the requirements for operation, espe-cially ionization for the magnetic processes, and heat-ing and cooling for the processes driven by gas pres-sure forces. We describe the distribution and strengthof the resulting flows and compare with the long-usedphenomenological α-picture, highlighting issues suchas grain transport and heating where the newer andmore-detailed models yield substantially different an-swers. We also discuss the links between magne-tized turbulence and magnetically-launched outflows,and between magnetized turbulence and hydrodynam-ical vortices. We end with a review of the prospects for

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detecting specific signatures of the flows in the next fewyears.

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ANGULAR MOMENTUM EVOLUTION OFYOUNG LOW-MASS STARS AND BROWNDWARFS: OBSERVATIONS AND THEORY[prog]J. Bouvier, S. Matt, S. Mohanty, A. Scholz, K.Stassun, C. Zanni

Spectacular progress has been made, both on the ob-servational and theoretical sides, on the issue of theangular momentum evolution of young stellar objectssince PPV. On the observational side, thousands ofnew rotational periods have been derived for stars overthe entire mass range from solar-type stars down tobrown dwarfs at nearly all stages of evolution betweenbirth and maturity. The picture we have of the rota-tional evolution of low- mass and very low-mass starsand brown dwarfs has never been as well documentedas of today. On the theoretical side, recent years haveseen a renaissance in numerical simulations of mag-netized winds that are the prime agent of angular mo-mentum loss, new attempts have been made to under-stand how young stars exchange angular momentumwith their disks via magnetic interactions, and new in-sights have been gained on the way angular momen-tum is transported in stellar interiors. Our chapter willreview the latest developments which shed new lighton the processes governing the angular momentumevolution of young stars and brown dwarfs, and also

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provide important context for other PPVI chapters byexploring possible connections between the rotationalhistory of stars and the formation, migration and evo-lution of planetary systems (star-disk interaction, innerdisk warps and cavities, planet engulfment, irradiationof young planets, etc.). We aim at providing the mostcomplete review of both the emerging concepts and thelatest observational results regarding the angular mo-mentum evolution of young low-mass stars and browndwarfs.

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JETS AND OUTFLOWS FROM STAR TOCLOUD: OBSERVATIONS CONFRONTTHEORY [prog]A. Frank, S. Cabrit, T. Ray, H. Arce, J.Eislöffel, S. Lebedev, F. Bacciotti, M. Guedel,B. Nisini, J. Bally, P. Hartigan, A.C. Raga

In this review we focus on the role of jets and out-flows in the star formation process. Are jets/outflowsmerely an epiphenomenon associated with star forma-tion or do they play an important role in mediating thephysics of assembling stars both individually and in aglobal sense? To address our questions we focus onthe current state of observations and on the importantpoints of contact between these observations and the-ory. We review the Jet/Outflow phenomena by organiz-ing our questions into 3 length-scale domains: Sourceand Disk Scales (1-102AU) where the connection withprotostellar and disk evolution theories is paramount;Envelope Scales (102-105 AU) where the chemistryand propagation shed further light on the jet launchprocess, its variability and impact on the infalling enve-lope. Parent Cloud Scales (105-106 AU) where issuesof large scale feedback on the global star formationprocess become important. In addition to describingresults from established platforms like the HST (multi-epoch imaging and spectroscopy) we also review newresults from facilities that are currently coming on-line

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(ALMA, the Jansky Array (EVLA), e-MERLIN. In de-scribing these observations we look to the future andconsider the questions that these new facilities can ad-dress. We also review results on jet dynamics fromemerging field of High Energy Density Laboratory As-trophysics (HEDLA) that provide direct insights into the3-D dynamics of fully magnetized, hypersonic, radioac-tive outflows.

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THE DISPERSAL OF PROTOPLANETARYDISCS [prog]R. Alexander, I. Pascucci, S. Andrews, P.Armitage, L. Cieza

The evolution and eventual dispersal of protoplanetarydisks play crucial roles in planet formation. Viscous ac-cretion, due to turbulent transport of angular momen-tum, is the dominant driver of disk evolution in theseplanet-forming systems. However, it is clear that ac-cretion cannot be responsible for the final dispersal ofthese disks, as the accretion time-scales in their outerregions are orders of magnitude larger than observeddisk lifetimes. Some other mechanism(s) must insteadbe responsible for clearing protoplanetary disks. Themanner and time-scales of disk dispersal have impor-tant implications for planet formation, and as disk clear-ing halts planet migration it also has a strong influenceon the final architectures of planetary systems. In thischapter we review the theory and observations whichunderpin our understanding of protoplanetary disk dis-persal, and discuss the consequences of these resultsfor forming planetary systems.

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AN OBSERVATIONAL PERSPECTIVE OFTRANSITIONAL DISKS AROUND T TAURISTARS [prog]C. Espaillat, S. Andrews, N. Calvet, P.D’Alessio, J. Hashimoto, A. Kraus, S. Kraus,J. Muzerolle, J. Najita, Z. Zhu

Disks around T Tauri stars (TTS) are thought to be thesites of planet formation. However, many questions ex-ist concerning how the gas and dust in the disk evolveinto a planetary system. Observations of TTS may pro-vide insights and there are some objects in particularthat have gained increasing attention in this regard.These objects contain inner holes in their disks andhave been dubbed transitional disks (TDs). Some havespeculated that planets are responsible for carving outthe holes in these TDs and that they are in transitionbetween protoplanetary disks and post-planet buildingdisks (i.e., debris disks). Spitzer produced detailedspectral energy distributions (SEDs) that allowed us toinfer the radial structure of TDs in some detail, andalso pointed to the diversity of TD systems. The grow-ing sample of TDs opened up the possibility of demo-graphic studies, which are providing unique insights.More recently, Spitzer results have stimulated work withother facilities. There now exist sub-millimeter andnear-infrared (NIR) images that confirm large cavitiesin TDs. In addition, potential protoplanets have been

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detected in some of these disks. TDs are the strongestlink to planet formation around TTS to date and area key area to study if further progress is to be madeon understanding the initial stages of planet formation.Here we will look at key observational properties con-straining the dust and gas properties of TDs and com-pare them to the main disk clearing mechanisms pro-posed to date (i.e., photoevaporation, grain growth, andplanets).

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OBSERVATIONS, MODELING AND THE-ORY OF DEBRIS DISCS [prog]B. Matthews, G. Bryden, C. Eiroa, A. Krivov,M. Wyatt

Main sequence stars, like the Sun, are often found tobe orbited by circumstellar material that can be cate-gorised into two groups, planets and debris. The lat-ter is made up of asteroids, comets, as well as thedust derived from them, which makes debris discs ob-servable in thermal emission or scattered light. Thesediscs may persist over Gyrs through steady-state evolu-tion and/or may also experience sporadic stirring, ren-dering them atypically bright for brief periods of time.Most interestingly, they provide direct evidence that thephysical processes (whatever they may be) that act tobuild large oligarchs from micron-sized dust grains inprotoplanetary discs have been successful in a givensystem, at least to the extent of building up as sig-nificant a planetesimal population as that seen in theSolar Systems asteroid and Kuiper Belts. Such sys-tems are prime candidates to host even larger plane-tary bodies as well. The recent growth in interest in de-bris discs has been driven by observational work thathas provided statistics, resolved images and discover-ies of new classes of objects. These datasets, fromthe Spitzer Space Telescope and the Herschel SpaceObservatory in particular, but also from near-IR inter-

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ferometers, ALMA and the new submillimetre cameraSCUBA-2 provide an unprecedented census of the hot,warm and cold components of debris discs, in manycases resolving the emission. Since 2005, the fieldhas gone from just over a dozen resolved discs at anywavelength to resolution of over 70 discs with Herschelalone, many at multiple wavelengths, a major observa-tional step forward. ALMA will be able to provide obser-vations with resolutions comparable to optical facilities,which promises to significantly impact our understand-ing of the substructure of debris discs, and potentiallyprovide a window into the planetary systems with whichthey co-exist. The interpretation of this vast and ex-panding dataset has necessitated significant advancesin debris disc theory. Application of this theory has ledto the realization that such observations provide a pow-erful diagnostic that can be used not only to refine ourunderstanding of debris disc physics, but also to chal-lenge our understanding of how planetary systems formand evolve.

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THE MULTIFACETED PLANETESIMALFORMATION PROCESS [prog]A. Johansen, J. Blum, H. Tanaka, C. Ormel,M. Bizzarro, H. Rickman

Accumulation of dust and ice into planetesimals is animportant step in the planet formation process. Plan-etesimals are the seeds of both terrestrial planets andthe solid cores of gas and ice giants. Left-over plan-etesimals in the form of asteroids, Kuiper belt objectsand comets provide a unique record of the state ofthe solar system during formation, while debris fromplanetesimal collisions around other stars signpoststhat the planetesimal formation process, and henceplanet formation, is ubiquitous in the Galaxy. Plan-etesimal formation extends from dust to sizes whichcan undergo run-away accretion, the latter rangingfrom 1 km to several thousand km dependent ongravitational torques from the turbulent gas. Pre-planetesimals face many barriers during this growth,arising mainly from inefficient sticking, fragmentationand radial drift. Two promising growth pathways arecoagulation-fragmentation, where particles grow largerby sweeping up collisional fragments, and fluffy growth,where particle cross sections and sticking are en-hanced by a low internal density. A wide range of par-ticle sizes, from mm to m, experience concentrationevents in the turbulent gas flow. Overdense regions

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can fragment gravitationally into bound particle clusterswith typical masses equivalent to planetesimals of 100to 1000 km sizes. We propose a hybrid model wheredust growth starts unaided by self-gravity but later pro-ceeds inside self-gravitating particle clumps to yield thefinal initial mass function of planetesimals.

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EARLY THERMAL EVOLUTION OF PLAN-ETESIMALS AND ITS IMPACT ON PRO-CESSING AND DATING OF METEORITICMATERIAL [prog]H.-P. Gail, D. Breuer, T. Spohn, T. Kleine, M.Trieloff

Radioisotopic ages for meteorites and their compo-nents provide constraints on the evolution of smallbodies: Timescales of accretion, thermal and aque-ous metamorphism, differentiation, cooling and impactmetamorphism. Realising that the decay heat of short-lived nuclides (e.g. 26Al, 60Fe), was the main heatsource driving differentiation and metamorphism, ther-mal modeling of small bodies is of utmost impotrance toset individual meteorite age data into the general con-text of the thermal evolution of their parent bodies, andto derive general conclusions about the nature of plan-etary building blocks in the early solar system. As ageneral result, modelling easily explains that iron mete-orites are older than chondrites, as early formed plan-etesimals experienced a higher concentration of short-lived nuclides and more severe heating. However, coreformation processes may also extend to 10 Ma afterCAIs. A general effect of the porous nature of the start-ing material is that relatively small bodies (< few km)will also differentiate if they from within 2 Ma after CAIs.A particular interesting feature to be explored is the

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possibility that some chondrites may derive from theouter undifferentiated layers of asteroids that are differ-entiated in their interiors. This could explain the pres-ence of remnant magnetization in some chondrites dueto a planetary magnetic field.

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TERRESTRIAL PLANET FORMATION ATHOME AND ABROAD [prog]S. Raymond, E. Kokubo, A. Morbidelli, R.Morishima, K. Walsh

We review the state of the field of terrestrial planet for-mation with the goal of understanding the formation ofthe inner Solar System and low-mass exoplanets. Wereview the dynamics and timescales of accretion fromplanetesimals to planetary embryos and from embryosto terrestrial planets. We discuss radial mixing and wa-ter delivery, planetary spins and the importance of pa-rameters regarding the disk and embryo propertis. Nextwe connect accretion models to exoplanets. We firstreview models for the growth of hot Super Earths by insitu accretion or inward migration. We show how ter-restrial planet formation is altered in systems with gasgiants, in particular by the mechanisms of giant planetmigration and dynamical instabilities. Standard modelsof terrestrial accretion fail to reproduce the inner So-lar System, and we show how the “Grand Tack” modelsolves this problem using ideas first developed to ex-plain the giant exoplanets. Finally, we discuss the keyingredients missing in the current generation of simula-tions.

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FORMATION OF BROWN DWARFS VS GI-ANT PLANETS: CONFRONTING THEORYWITH OBSERVATIONS [prog]G. Chabrier, M. Janson, A. Johansen, R.Rafikov

The formation of brown dwarfs and gaseous planetsis one of the most debated issues in the general do-main of planet and star formation. These objects bydefinition lie in the overlapping domain between starsand low-mass planets. Finding out whether their forma-tion involves completely distinctive mechanisms or, onthe contrary, shares common processes remains a keyquestion fo fully understand structure formation overthe entire planetary and stellar regime. It is the aimof the present review to address these questions andto find out whether or not we have reasonably robustanswers. We will critically examine our present under-standing of brown dwarf and giant planet formation andwill confront the predictions of the various suggestedformation scenarios with observations. As the outcomeof these confrontations, we will try to determine what isor are the common and different dominant mechanismsfor brown dwarf and planet formation and whether onecan provide reasonably sound answers to the abovequestions. Finally, we will identify possible observa-tional diagnostics to distinguish these two different pop-ulations as imprints from their formation mechanism,

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providing guidance for future observational strategies.

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GIANT PLANET FORMATION, EVOLU-TION, AND INTERNAL STRUCTURE

[prog]R. Helled, P. Bodenheimer, Y. Alibert, M.Podolak, S. Nayakshin, A. Boley, A. Boss, J.Fortney, F. Meru, L. Mayer

The large number of detected extrasolar giant planetsoffers the opportunity to improve our understanding ofthe formation mechanism, evolution, and interior struc-ture of gas giant planets. The two main models for giantplanet formation are known as core accretion and diskinstability. There are substantial differences betweenthese formation models, including formation timescale,favorable formation location, ideal disk properties forplanetary formation, early evolution, planetary compo-sition, etc. First, we summarize the two models includ-ing their substantial differences, advantages, and dis-advantages. We present the predicted planetary com-position in each model, and suggest how theoreticalmodels should be connected to available (and future)data. We next summarize current knowledge of the in-ternal structures of solar- and extrasolar- giant planets.Finally, we suggest the next steps to be taken in solarand extrasolar giant planet exploration.

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PLANET-DISC INTERACTIONS AND EARLYEVOLUTION OF PLANETARY SYSTEMS[prog]C. Baruteau, A. Crida, B. Bitsch, J. Guilet,S.-J. Paardekooper, F. Masset, R. Nelson, W.Kley, J. Papaloizou

The great diversity of extrasolar planetary systems haschallenged our understanding of how planets form, andhow their orbits evolve as they form. Among the var-ious processes that may account for this diversity, thegravitational interaction between planets and their par-ent protoplanetary disc plays an inevitable role in shap-ing young planetary systems by causing considerablemobility. Planet-disc forces are large, and the char-acteristic times for the evolution of planets orbital ele-ments are much shorter than the lifetime of protoplane-tary discs. The determination of such forces is difficult,because it involves many physical mechanisms and itrequires a detailed knowledge of the disc structure. Theintense research of the past few years, with the explo-ration of many new avenues, represents a very signif-icant improvement on the state of the discipline pre-sented in PPV. The objective of this chapter is to re-view current understanding of planet-disc interactions.Emphasis is placed on mechanisms capable of slowingdown, stalling or reversing planet migration, which mayhelp account for the exoplanets diversity. We then ad-

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dress how well global models of planet formation andmigration are able to match observations of extrasolarplanets.

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PLANET POPULATION SYNTHESIS [prog]W. Benz, S. Ida, Y. Alibert, D. Lin, C. Mordasini

The common existence of exoplanets and their richstructural and dynamical diversity indicates that theirformation is a robust process, their evolution is drivenby many competing physical processes and their des-tiny is determined by a wide range of boundary condi-tions. Population synthesis models provide a useful toolfor the interpretation of exoplanets’ present-day prop-erties and the understanding of the dominant effects ateach stages of their evolutionary paths. They also gen-erate testable predictions which can be used to guidefuture observational strategy and model upgrades. Theconstruction of comprehensive models and the explo-ration of the vast parameter space is still in a develop-mental stage. We review here the present status of thisapproach including 1) an exhaustive account of poten-tially relevant physical processes, 2) a summary of thequantitative prescriptions which are introduced to ap-proximate the consequence of each effect, 3) a reporton various computational methods to simulate statisti-cal distributions, and 4) a compilation of the assumedboundary and initial conditions. We outline some out-standing theoretical uncertainties and accentuate theneed of some critical observational calibrations. Weconfront the results of some simulated planetary cen-sus with existing data and present both the successful

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reproduction and disagreements between current ver-sions of population synthesis models and observations.We identify which results can be considered reliableand which are still based on unknown processes and/orparameters. Finally, we suggest future theoretical andobservational investigations that can improve the relia-bility of the models.

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NEW EXOPLANETARY SYSTEMS [prog]D. Fischer, J. Yee, J. Sahlmann, B. Macintosh,G. Laughlin, S. Mahadevan, A. Howard

These are still the early days of exoplanet discov-ery. Astronomers are beginning to model the atmo-spheres and interiors of exoplanets and have devel-oped a deeper understanding of processes of planetformation and evolution. However, we have yet to mapout the full complexity of multi-planet architectures or todetect Earth analogues around nearby stars. Reachingthese ambitious goals will require continued improve-ments in instrumentation and analysis tools. In thischapter, we provide an overview of five observationaltechniques that are currently employed in the detectionof exoplanets: optical and IR Doppler measurements,transit photometry, microlensing, astrometry and directimaging. We provide a basic description of how thetechniques work and discuss forefront development tokeep these methods productive. We highlight the ob-servational limitations and synergies of each methodas well as connections to future space missions.

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EXOPLANETARY ATMOSPHERES [prog]N. Madhusudhan, H. Knutson, J. Fortney, T.Barman

The study of exoplanetary atmospheres is one of themost exciting and dynamic frontiers in astronomy. Overthe past two decades ongoing surveys have revealedan astonishing diversity in the planetary masses, radii,temperatures, orbital parameters, and host stellar prop-erties of exoplanetary systems. We are now movinginto an era where we can begin to address fundamen-tal questions concerning the diversity of exoplanetarycompositions, atmospheric and interior processes, andformation histories, just as have been pursued for so-lar system planets over the past century. Exoplane-tary atmospheres provide a direct means to addressthese questions via their observable spectral signa-tures. In the last decade, and particularly in the lastfive years, tremendous progress has been made in de-tecting atmospheric signatures of exoplanets throughphotometric and spectroscopic methods using a vari-ety of space-borne and/or ground-based observationalfacilities. These observations are beginning to pro-vide important constraints on a wide gamut of atmo-spheric properties, including pressure-temperature pro-files, chemical compositions, energy circulation, pres-ence of clouds, and non-equilibrium processes. Thelatest studies are also beginning to connect the inferred

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chemical compositions to exoplanetary formation con-ditions. In the present chapter, we review the mostrecent developments in the area of exoplanetary at-mospheres. Our review covers advancements in bothobservations and theory of exoplanetary atmospheres,and spans a broad range of exoplanet types (gas gi-ants, ice giants, and super-Earths) and detection meth-ods (transiting planets, direct imaging, and radial ve-locity). A number of upcoming planet-finding surveyswill focus on detecting exoplanets orbiting nearby brightstars, which are the best targets for detailed atmo-spheric characterization. We close with a discussion ofthe bright prospects for future studies of exoplanetaryatmospheres.

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PLANETARY INTERNAL STRUCTURE[prog]I. Baraffe, G. Chabrier, J. Fortney, C. Sotin

This chapter will review the most recent advancementon the topic of terrestrial and giant planets interiors, in-cluding solar system and extra-solar objects. Startingfrom an observed mass-radius diagram for all knownplanets in the Universe, we will discuss the varioustypes of planets appearing in this diagram and de-scribe internal structures for each types. The reviewwill summarize the status of theoretical and experimen-tal works performed in the field of equation of states(EOS) for materials relevant to planetary interiors andwill address the main theoretical and experimental un-certainties and challenges. It will discuss the impact ofnew EOS on interior structures and bulk compositiondetermination. We will discuss important dynamicalprocesses which strongly impact the interior and evo-lutionary properties of planets (plate tectonics, convec-tion, semiconvection) and describe non standard mod-els recently suggested for our Giant planets. We willaddress the case of short-period, strongly irradiated ex-oplanets and discuss some of the physical mechanismswhich have been suggested to explain their anoma-lously large radius. We will also address key ques-tions in the context of a Protostars and Planets con-ference: Can we easily link interior structures and for-

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mation processes? Can we distinguish a brown dwarffrom a planet? We will finally discuss future missionswhich will advance our knowledge on planetary interiorstructures.

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THE LONG-TERM DYNAMICAL EVOLU-TION OF PLANETARY SYSTEMS [prog]M. Davies, F. Adams, P. Armitage, J. Cham-bers, E. Ford, A. Morbidelli, S. Raymond, D.Veras

This talk/chapter concerns the long-term dynamicalevolution of planetary systems from both theoreticaland observational perspectives. We begin by dis-cussing the planet-planet interactions at play in our ownSolar System. We then describe how these changewhen one considers more tightly-packed planetary sys-tems with some systems becoming dynamically unsta-ble as planet-planet interactions grow leading to strongencounters and ultimately either ejections or collisionsof planets. We first discuss the basic physical pro-cesses at play and then consider how these processesapply to extrasolar planetary systems and what con-straints are provided by observed systems. The pres-ence of a residual planetesimal disc can lead to plan-etary migration and may cause instabilities induced byresonance crossing, although such discs may also sta-bilise a planetary system. The crowded birth environ-ment of a planetary system can have a significant im-pact: close encounters and binary companions may actto destabilise a system. In particular, in the latter casethe Kozai mechanism may place planets on extremelyeccentric orbits which may later circularise to produce

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hot jupiters.

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SAMPLES OF THE SOLAR SYSTEM: RE-CENT DEVELOPMENTS [prog]A.M. Davis, C. M. O’D. Alexander, F.J. Ciesla,M. Gounelle, A.N. Krot, M. Petaev, T. Stephan

We review recent studies of the isotopic, chemical, andphysical properties of materials in meteorites and re-turned to Earth by spacecraft and their implications forthe early history of the solar system.

Perhaps the most remarkable discovery, fromthe Genesis mission that sampled the solar wind, is thatthe oxygen isotopic composition of the Sun is about 5%lower in 18O/16O and 17O/16O than the Earth, Moon,Mars and meteorite parent bodies. The origin of thisdifference continues to be hotly debated, but there areprofound implications for processing and transport ofmaterials within the solar nebula. The Sun is evenmore depleted in 15N/14N, by about 40%, comparedto the Earths atmosphere. Isotopic self-shielding ofCO and N2 in the UV may explain both observations,but this is far from being proven. Self-shielding mayhave occurred in the solar nebula, either near the Sunor at the surface of the solar nebula, or could havebeen inherited from the natal molecular cloud. Deu-terium/hydrogen ratios are now known in a numberof solar system objects, through both direct measure-ments and remote sensing. The relatively low D/H ra-tios of water in carbonaceous chondrites indicate that

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they formed closer to the Sun than comets and Ence-ladus, in conflict with some predictions of the Nice andGrand Tack models. The bulk hydrogen and nitrogenisotopic compositions and volatile element abundancesof the CI and CM carbonaceous chondrites suggestthat they are the likely sources of the volatiles accretedby the terrestrial planets.

There has been considerable activity in thestudy of short-lived radionuclides in the early solar sys-tem. Careful isotopic study of a variety of meteoriteshas lowered the early solar system 60Fe/56Fe ratio bynearly two orders of magnitude from the value of tenyears ago, weakening the case for a supernova trig-ger for solar system formation. The 235U/238U ratio hasbeen found not to be constant in calcium-, aluminum-rich inclusions (CAIs), so that both uranium and leadisotope ratios must be measured to obtain absolutechronology of early solar system events. The limiteddataset of uranium-corrected Pb-Pb dates now giveconsistent relative time differences with the 182Hf-182Wand 53Mn-53Cr systems. The 26Al-26Mg system hasbeen used to show that CAIs in CV chondrites formedwithin a remarkably short period of time, perhaps onlya few thousand years. There is also clear evidence that26Al had a stellar origin (the nature of stellar source,SNII, AGB, or WR remains unclear) and was heteroge-neously distributed within the solar system, but the fullimplications of this heterogeneity are yet to be worked

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out. Uranium-corrected Pb-Pb absolute dating showsthat chondrule formation started contemporaneouslywith CV chondrite CAI formation and lasted for at least3 Ma. How pristine mm- to cm-sized CAIs and early-formed chondrules were stored for 3 Ma before accre-tion of meteorite parent bodies remains an outstandingproblem.

Chondrule formation continues to be a mystery,but formation in the solar nebula by transient heatingdue to shock remains popular. There is increasing in-terest in chondrule formation by asteroid collisions, butthe only clear case for this are the metal and silicatechondrules in the rare CB chondrites that appear tohave formed in an impact plume. Enstatite chondriteshave long been a puzzle, because reduced phasessuch as magnesium and calcium sulfides seem to re-quire condensation from a gas with C/O∼1, about twicethe solar ratio. New textural and compositional evi-dence and modeling suggests that enstatite chondritesformed in a way similar to other chondrites but wereprocessed in a hydrogen-poor, sulfur-rich environmentunder near-nebular redox conditions.

Dust from comet Wild 2 returned to Earth bythe Stardust spacecraft revealed several surprises. Thedust has abundant refractory material, including CAIsand chondrules, indicating high temperature process-ing in the inner solar system and is very similar to chon-drites in overall chemical composition. The abundance

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of presolar grains and amorphous materials appear tobe low, but these materials are easily destroyed by highvelocity capture in aerogel. With the lack of hydrousminerals and its mostly fine-grained nature, Wild 2 dustresembles chondritic porous interplanetary dust parti-cles (IDPs), often interpreted as cometary IDPs, withsome added coarse-grained refractory mineral grains.The high abundance of refractory materials implies thatoutward radial transport in the solar nebula was muchmore effective than previously recognized.

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DEUTERIUM FRACTIONATION: THE ARI-ANE THREAD FROM THE PRE-COLLAPSEPHASE TO METEORITES AND COMETSTODAY [prog]C. Ceccarelli, P. Caselli, D. Bockelee-Morvan,O. Mousis, S. Pizzarello, F. Robert, D. Se-menov

Once upon a time, there was a small cold condensationof gas and dust in an interstellar cloud broken into sev-eral clumps and filaments of different masses and di-mensions. Then, about 4.5 billions years ago, the con-densation became the Solar System. What happenedto that primordial condensation? When, why and howdid it happen?

Answering these questions involves putting to-gether all of the information that we have on the presentday solar system bodies and micro particles. But often,this is not enough: combining it with our understand-ing of the formation process of solar type stars in ourGalaxy largely enhances our capacity to reconstructwhat happened to ours. In this respect, the chemi-cal composition of matter during the formation processis an extremely useful and, sometimes, almost uniquetool. One specific example is offered by the molec-ular deuteration, namely the ratio between the abun-dances of the H- and D-bearing isotopologues of the

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same species. The few examples that we will givein the following show the huge diagnostic power con-tained in the measured molecular deuteration, a powerthat we plan here to fully review and exploit, bringingtogether our knowledge on interstellar astrochemistry,solar type star and planet formation, comets and solarsystem small bodies, and meteoritic material.

Our first example is about the Earth water.Terrestrial water that possesses an enhancement ofHDO with respect to H2O by about one order of mag-nitude with respect to the D/H elemental abundance(1.6x10-5). On the on other hand, bulk mineralogicalcomposition of the Earth’ crust is remarkably similarto that of most primitive chondritic meteorites, whichhave formed at ”dry”, water-free conditions. Sincecomets and some of carbonaceous chondrites showwater deuteration of the same order of magnitude, itwas suggested that the Earth water was mostly deliv-ered by comets and/or icy bodies raining on the earlyEarth. The thesis is debatable and debated, and we willreview all the discussion on the subject. Nonetheless,the example means to show how the water deuterationin terrestrial water brings us back to the primitive Earthhistory and likely even earlier than that. What more, therecent discovery by Herschel of the HDO/H2O abun-dance ratio in comet 103P/Hartley2, twice lower thanthe value measured in comets believed to originate far-ther from the Sun, has triggered a debate on the very

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origin of the comets in the Solar System and on thethermal structure of the Solar Nebula, requiring as wella new class of models. Again, we will review the on go-ing debate. Our second, notable example is providedby the discoveries that meteoric material is highly en-riched in deuterium. This is true for soluble and insol-uble material, as well as for clay minerals in carbona-ceous meteorites. How this high degree of deutera-tion was acquired? Through inheritance from previ-ous epochs or at the latest phases of the Solar Neb-ula formation? If the latter is true, where and how?The lessons that we have learned from the studies ofmolecular deuteration occurring during the pre-stellarto proto-planetary phases will enormously help to un-derstand the origin of the organic material and clay min-erals in meteorites and, consequently, how the SolarSystem formed.

In this Chapter we will review the present un-derstanding of the deuteration process across the vari-ous phases of a solar type star and planet formation,and compare it with the observations and models ofvarious objects of the Solar System. We will use thedeuteration as the Ariadnes thread. The legend saysthat he thread was given by Ariadne to Theseus to getout fromŁa difficult situation, the Minotaur’s labyrinth.Theseus followed the thread that he had previously un-rolled to get into the labyrinth to get out of it. Simi-larly, deuteration can help us to find the way out of the

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labyrinth of what happened to our Solar System.

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ASTROPHYSICAL CONDITIONS FORPLANETARY HABITABILITY [prog]M. Güdel, R. Dvorak, N. Erkaev, J. Kasting, M.Khodachenko, H. Lammer, E. Pilat-Lohinger,H. Rauer, I. Ribas, B. Wood

With the discovery of hundreds of exoplanets and apotentially huge number of Earth-like planets waitingto be discovered, the conditions for their habitabilityhave become a focal point in exoplanetary research.The classical picture of habitable zones primarily re-lies on the stellar flux allowing liquid water to exist onthe surface of an Earth-like planet with a suitable atmo-sphere. However, numerous further stellar and plane-tary properties constrain habitability. Apart from ”geo-physical” processes depending on the internal structureof a planet, a complex array of astrophysical factorsadditionally determine habitability. Among these, vari-able stellar UV, EUV, and X-ray radiation, stellar andinterplanetary magnetic fields, ionized winds, and en-ergetic particles control the constitution of upper plane-tary atmospheres and their physical and chemical evo-lution. Short- and long-term stellar variability necessi-tates full time-dependent studies to understand plan-etary habitability at any point in time. Furthermore,dynamical effects in planetary systems and transportof water to Earth-like planets set fundamentally impor-tant constraints. We will review these astrophysical

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conditions for habitability under the crucial aspects ofthe long-term evolution of stellar properties, the con-sequent extreme conditions in the early evolutionaryphase of planetary systems, and the important interplaybetween properties of the host star and its planets.

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Posters

[back to start of document]

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How to navigate among the posters

Poster Sessions: The posters are dividedinto two groups: the ones in the first half ofthe week (from Monday morning to Wednes-day lunchtime) and the ones in the second halfof the week (from Wednesday late afternoonto Saturday morning). You can see from theposter number which session the poster is in(see below).

Poster numbers: The poster numbers con-sist of 3 parts: The session in which the posteris planned (1 or 2), the room in which it is lo-cated (room S, B, H, G or K, see map of thefirst elevated floor of the conference center be-low – the letters stand for the names of therooms), and finally the 3-digit poster numberwithin that room. So poster 2B040 is in ses-sion 2 (second half of the week), in room B(the Ballroom), poster number 40.

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Minimaps: The icons below the title and au-thor (like the one shown here)

are in fact minuscule maps of the conferencecenter (first elevated floor) with the posterrooms (compare to the more realistic and de-tailed map below). The zigzag lines are theposterboard arrangements. The arrow pointsto where the poster is located.

Electronic navigation: In the electronic PDFversion of this PPVI companion you can clickon all blue hyperrefs. They allow you to navi-gate back and forth from overview lists to theposter abstracts and vice versa. Of courseyou can also use the search functionality ofyour PDF viewer to search for keywords ornames. Clicking on an email address (or onthe blue bullets in the participant list) will startan email to that person, making it easier to ar-range a meeting with that person.

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Poster Topic List

Topic 01 GENERAL

Topic 02 MOLECULAR CLOUDS: CHEMISTRY

Topic 03 MOLECULAR CLOUDS: IRDCS AND FIL-AMENTS

Topic 04 MOLECULAR CLOUDS: CORES

Topic 05MOLECULAR CLOUDS: FORMA-TION, TURBULENCE AND EVOLU-TION/FEEDBACK

Topic 06 MOLECULAR CLOUDS: GENERAL

Topic 07 MASSIVE STAR FORMATION: CHEM-ISTRY

Topic 08 MASSIVE STAR FORMATION: CLUS-TERS

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Topic 09 MASSIVE STAR FORMATION: ACCRE-TION DISKS

Topic 10 MASSIVE STAR FORMATION: HII RE-GIONS

Topic 11 MASSIVE STAR FORMATION: YSOS

Topic 12 MASSIVE STAR FORMATION: GEN-ERAL

Topic 13 YSO: CHEMISTRY

Topic 14 YSO: COLLAPSE

Topic 15 YSO: FORMATION OF PROTOSTELLARDISKS, FIRST HYDROSTATIC CORE

Topic 16 YSO: SURVEYS

Topic 17 YSO: VARIABILITY

Topic 18 YSO: GENERAL

Topic 19 STAR FORMATION: CLUSTERS

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Topic 20 STAR FORMATION: STAR FORMATIONREGIONS

Topic 21 STAR FORMATION: TRIGGERED SF

Topic 22 STAR FORMATION: GENERAL

Topic 23 JETS AND OUTFLOWS: LAUNCHING,JET-DISK CONNECTION

Topic 24 JETS AND OUTFLOWS: PROPER MO-TION, VARIABILITY, EVOLUTION

Topic 25 JETS AND OUTFLOWS: ROTATION

Topic 26 JETS AND OUTFLOWS: SURVEYS

Topic 27 JETS AND OUTFLOWS: GENERAL

Topic 28 STARS: BROWN DWARFS

Topic 29 STARS: BINARIES AND MULTIPLES

Topic 30 STARS: CLUSTERS

Topic 31 STARS: GENERAL

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Topic 32 GENERAL

Topic 33 PROTOPLANETARY DISKS: ACCRE-TION

Topic 34 PROTOPLANETARY DISKS: CHEM-ISTRY

Topic 35 PROTOPLANETARY DISKS: DISPER-SAL

Topic 36 PROTOPLANETARY DISKS: DUST

Topic 37 PROTOPLANETARY DISKS: DYNAMICS,HYDRODYNAMICS, TURBULENCE

Topic 38 PROTOPLANETARY DISKS: EVOLU-TION

Topic 39 PROTOPLANETARY DISKS: STRUC-TURE

Topic 40 PROTOPLANETARY DISKS: SURVEYS

Topic 41 PROTOPLANETARY DISKS: TRANSI-TION DISKS

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Topic 42 PROTOPLANETARY DISKS: VARIABIL-ITY

Topic 43 DEBRIS DISKS

Topic 44 PLANET FORMATION: CHEMISTRY

Topic 45 PLANET FORMATION: DUST COAGU-LATION

Topic 46 PLANET FORMATION: PARTICLETRAPS AND DUST TRANSPORT

Topic 47 PLANET FORMATION: FORMATION OFPLANETESIMALS

Topic 48 PLANET FORMATION: PLANETARYSYSTEMS AND ORBITAL DYNAMICS

Topic 49 PLANET FORMATION: TERRESTRIALPLANETS

Topic 50 PLANET FORMATION: GAS GIANTPLANETS

Topic 51 PLANET FORMATION: PLANET-DISK IN-TERACTION AND MIGRA