Here you should find the abstracts of all registered participants (version 23rd Oct, not the latest->Program):
Abstracts German-Japanese meeting Note: Schedule: Alexander "Sasha" Krivov (can only come Friday) 1. Jürgen Blum Per aspera ad planetas – there is hope that we will finally understand planetesimal formation SESSION: PLANET FORMATION (Planetesimals) After decades of modeling and experimental work on the growth from microscopically small dust particles to multi-kilometer-sized planetesimals, there are currently three competing scenarios on the market: (1) coagulation of dust to pebble-sized agglomerates, followed by sequences of instabilities which concentrate the dust particles until gravitation instability forms planetesimals, (2) direct collisional growth over the bouncing and fragmentation barriers to planetesimal sizes through the effect of mass transfer in collisions between very large and very small bodies, and (3) direct collisional growth without any barrier to planetesimal sizes, aided by the enhanced stickiness of sub-µm-sized water- ice particles. In my presentation, I will present these three planetesimal-formation models, including the empirical evidence from laboratory experiments they are based upon, and will also discuss the pros and cons of them as well as observational constraints, which can help to solve the mystery of planetesimal formation. 2. Jeroen Bouwman, MPIA Characterization of planetery atmospheres from space. SESSION: EXO-PLANETS (Atmospheres) The Hubble and Spitzer Space Telescopes have revolutionized the observational characterization of exo-planets by detecting infrared emission and absorption from hot Jovian atmospheres. These detections have stimulated extensive theoretical work on the atmospheric structure and emission of these planets. Constraining the model predictions for infrared emission from hot Jovian atmospheres is an important motivation for current and future observing programs. Spectral characterization of hot Jovian exo-planets is a high priority and is essential for understanding atmospheric composition and properties. In this presentation I discuss the current observational capabilities with Spitzer and HST and give an outlook into future JWST observations. 3. Wolfgang Brandner Characterisation of cool brown dwarf and planetary atmospheres SESSION: EXO-PLANETS (Atmospheres) Today more than 1,500 exoplanets are known. The majority are giant planets detected by radial velocity or transit observations, yielding information on exoplanet masses, orbital periods, and bulk densities (and hence average compositions). The determination of the atmospheric properties like overall metallicity, chemical composition and mixing, vertical temperature profile, and cloud coverage and constituents is considerably more challenging. Directly imaged planets offer the advantage that they are at relatively large distances from their host star, and hence are subject to considerably less radiative forcing than closer-in planets. In addition, unlike the majority of the transiting planets, directly imaged planets are also more readily accessible at all orbital phases. In this talk I will present some of our recent observational results, which enable us to test atmospheric models, and to constrain atmospheric properties of cool brown dwarfs and exoplanets. 4. Cornelis Dullemond Observing dust traps with ALMA SESSION: DISKS (Observations) Abstract: Among the most striking observations of protoplanetary disks with the new ALMA array is the lopsided ring structures in a number of transition disks. The most famous examples at present are the IRS 48 disk in which there is a very bright kidney shaped continuum blob on one side of the star, and the HD 142527 disk in which there is a banana shaped half-ring around the star. In both cases the emission originates from dust grains. I will discuss a theoretical interpretation of these lopsided structures in terms of a huge Rossby vortex in which dust particles are trapped. Dust trapping in vortices was predicted almost 2 decades ago and now appears to be observed in real disks. However, further observational tests, in particular with the new longer baselines of ALMA, will have to be conducted to confirm this. 5. Hidenori Genda Collisions in Extrasolar Systems SESSION: PLANET FORMATION (Protoplanets) Collision is a fundamental process of planet formation in extrasolar planetary systems as well as our solar system. Here we focus on many types of collisions between planetesimals, protoplanets, super-Earths, and gas giant planets. We will show our recent results of numerical simulations. For example, in collisions between planetesimals, we re-evaluated the critical impact energy for catastrophic disruption, which affects the growth of protoplanets, and revealed that it was about a half order of magnitude smaller than the previous studies expected. Some types of collisions between super-Earths or gas giant planets would change their compositions, such as water-rock or envelope-core ratios. 6. Jun Hashimoto Near-Infrared Imaging Observations of Transitional Disks by the Subaru/ SEEDS project SESSION: DISKS (Observations) SEEDS is a strategic project in the Subaru telescope exploring exoplanets and circumstellar disks around 500 stars in the near-infrared wavelengths. The project has started in 2009 and will be completed in this year. Here, we review the project and summarize the major results especially in the survey of protoplanetary disks by near-infrared polarimetric imaging. In observing protoplanetary disks, we mainly focus on transitional disks known as a protoplanetary disk with a cavity in a central region of a disk. Disk-planet interaction would be one of intriguing interpretations potentially responsible for such a cavity-stracture. Thus, transitional disks would be unique samples for understanding planet formation in a disk. As results of tens of observations in transitional disks, we have resolved fine structures in disks such as spirals, gaps, and dips at a radius of tens AU possibly due to gravitational interactions with unseen planet(s). These results may support planet formation at a wide orbit, e.g., GJ 504 b at 43 AU. We also found differences in structures of a cavity observed in the near-infrared and (sub-)millimeter wavelengths, i.e., a clear cavity in (sub-)millimeter wavelengths while no cavity in near-infrared wavelengths. The different behavior between small (sub-micron size) and large (millimeter size) dust grains at the cavity-wall sculpted by planet(s) could result in observing differences. Finally, we mention our scientific activities in ALMA based on SEEDS data. 7. Artie P. Hatzes Detecting Short-period, Earth-mass planets in the Presence of Activity Noise SESSION: EXO-PLANETS (Detection) The radial velocity (RV) jitter due to stellar activity can often be the limiting factor in our ability to detect Earth-mass planets with the Doppler method. For highly active stars this intrinsic variability can have amplitudes of a few to tens of m/s. I introduce the Floating Chunk Offset method for detecting short-period low mass exoplanets in the presence of activity noise. In this method RV data with good temporal sampling are divided into chunks with time intervals shorter than the expected periods from activity. An orbital fit is then made at a given period allowing the velocity offsets in the chunks to vary. This method has been employed on transiting planets with known periods. The FCO method can also be used as a periodogram that acts as an effective "low-pass" filter of activity noise thus allowing planets with unknown orbital periods to be detected. The FCO method is applied to RV data for the transiting rocky planets CoRoT-7b and Kepler-78b. The resulting K-amplitude due to Kepler-78b is slightly lower than published values and implies a planet mass of 1.31 ± 0.24 M_Earth. The nominal planet density of 4.5 ± gm cm^-3 is consistent with a low iron structure (Moon-like) although the error is large enough to encompass an Earth-like structure. More RV data are needed to distinguish between the models. 8. Th. Henning, J. Bouwman, D. Semenov. T. Albertsson Water: From Disks to Planets SESSION: DISKS (Observations) I will shortly summarize recently obtained observational constraints on the distribution of water vapour in protoplanetary disks. The talk will present the spectroscopic discovery of water ice in disks around Herbig Ae stars at far- infrared wavelength with Herschels. We will use this discovery to constrain the formation pathway of water ice. In addition, I will discuss the origin of water on Earth using chemical models for the solar nebula including turbulent mixing. 9. Shigeru Ida Orbital evolution of clumps formed by disk instability -implications for wide separation direct-imaged Jupiters SESSION: PLANET FORMATION (Fragmentation) We have studied orbital evolution of clumps formed by disk instability in outer disk regions. The detection of wide separation jupiters by direct imaging challenges conventional core accretion model and revived disk instability model has been proposed for formation of these planets. However, hydrodynamical simulations suggest that the clumps formed by disk instability rapidly migrate inward. Because hydrodynamical simulations cannot follow the orbital evolution on long timescales, we followed the evolution by orbital calculation, taking into account dynamical friction and disk turbulence. We will show that final orbital distributions of the clumps to discuss origin of wide separation direct-imaged Jupiters. 10. Masahiro Ikoma Bulk and atmospheric composition of transiting low-mass exoplanets and their origins. SESSION: EXO-PLANETS (Atmospheres) Recent transit measurements of exoplanets have revealed that there are a significant number of low-density low-mass planets with short orbital periods. I will talk about our recent theoretical studies of accumulation and secondary loss of the atmosphere of short-period low-mass planets. Also, to gain deeper understanding of the composition of short-period exoplanets, we have recently done modeling of the atmosphere and, furthermore, performed multi-wavelength transit measurements with several Japanese telescopes. So I want to talk about our recent status of the characterization of the atmosphere of several transiting exoplanets. 11.Shu-ichiro Inutsuka The Formation and Early Evolution of Protoplanetary Disks: A Hybrid Scenario of Planet Formation SESSION: DISKS (Modelling) The formation and early evolution of protoplanetary disks are described in this talk. Recent advance in the modeling with resistive magneto-hydrodynamical codes with various numerical techniques has enabled our understanding on the formation of protostars with outflows/jets and the formation of protoplanetary disks in a self-consistent manner from molecular cloud cores. This provides improved description for the realistic environments for planet formation in the gaseous disks. We find that gaseous planetary-mass objects can be formed by gravitational instability in the regions that are de-coupled from the magnetic field and surrounded by the injection points of the magneto-hydrodynamical outflows during the formation phase of protoplanetary disks. Magnetic de-coupling enables massive disks to form and these disks are subject to gravitational instability, even at ~10 AU. The frequent formation of planetary mass objects in those disks suggests the possibility of constructing a hybrid scenario of planet formation, i.e., the rocky planets form later under the influence of the giant planets in the protoplanetary disk. Our recent N-Body simulations of the new scenario shows a new mechanism by which resultant rocky planets possibly gravitationally push the giant planet towards the central stars. This "crowding- out" mechanism may explain the observed lDiack of companion planets in HJ systems. 12. Viki Joergens The formation of free-floating planets SESSION: EXO-PLANETS (w. Disks?) We show that the coolest known object that is formed in a star-like mode is a free-floating planet. We discovered recently that the free-floating planetary mass object OTS44 (M9.5, ~12 Jupiter masses, age ~2 Myr) has significant accretion and a substantial disk. This demonstrates that the processes that characterize the canonical star-like mode of formation apply to isolated objects down to a few Jupiter masses. We detected in VLT/SINFONI spectra that OTS44 has strong, broad, and variable Paschen beta emission. This is the first evidence for active accretion of a free-floating planet. The object allows us to study accretion and disk physics at the extreme and can be seen as free-floating analog of accreting planets that orbit stars. Our analysis of OTS44 shows that the mass-accretion rate decreases continuously from stars of several solar masses down to free- floating planets. We determined, furthermore, the disk mass (30 Earth masses) and further disk properties of OTS44 through SED modeling based on far-IR Herschel data. We find that objects between 14 solar masses and 0.01 solar masses have the same ratio of the disk-to-central-mass of about 0.01. Our results indicate that OTS44 is formed like a star and suggest that the increasing number of young free-floating planets and ultra-cool field T and Y dwarfs are the low-mass extension of the stellar population. 13.Lisa Kaltenegger What can we really observe? Biosignatures on rocky planets and the observable concept of the Habitable Zone SESSION: EXO-PLANETS (Atmospheres) In recent literature several claims have been made on extension of the Habitable Zone as well as detectability or confusion on biosignatures on rocky planets. Using a versatile 1D atmosphere model I will show a range of observable biosignatures in transmission as well as emergent flux for a range of rocky planets from Mini- to Super-Earths in the Habitable zone and discuss the HZ concept. We will concentrate on recently discovered planets around cool stars as well as the range of changes in a planet’s atmosphere due to the host star. 14. Hajime Kawahara Characterization of Exoplanets with High-contrast and High-Dispersion Instruments on Extremely Large Telescopes SESSION: EXO-PLANETS (Detection) High-contrast instruments with future planned 30-40 m class telescopes such as TMT, GMT, and E-ELTs will expand our knowledge of exoplanets. I will talk about our recent study of characterization techniques of exoplanets assuming these instruments. One is the feasibility study of the oxygen 1.27 micron feature of planets in the HZ around the lath-type stars. We investigate the noise from terrestrial atmosphere for the 1.27 micron, especially night airglow of terrestrial oxygen. We found that its emissivity significantly decreases an order of magnitude by midnight. The future detectors for which the detection contrast is limited by photon noise can detect this feature (Kawahara+2012 ApJ 758, 13). We also consider an application of the high-contrast instruments to the spectroscopic detection of close-in planets (e.g. Brogi+2012 Nature 486, 502, Rodler+2012 ApJL 753,25) with the high-dispersion instruments. So far, CO and water have been detected for nearby hot Jupiters. The high-contrast instruments will extend the target to warm Juptiers and Neptune-size planets with the 1 mas rms tip-tilt correction (Kawahara+ ApJS submitted arXiv:1404.5712). The tip-tilt error is crucial for this type of observations. If we can correct the tip-tilt error within 0.3 mas (rms), we have ~30 times larger gain in the S/N. It will enable us to perform precise measurements of the planetary radial velocity, which can be used for detections of the planetary wind and rotation for the close-in planets(e.g. Kawahara ApJL 760, 13). 15.Hubert Klahr The Formation of Planetesimals in Starving Mode: Zonal Flows and Vortices in Circumstellar Disks SESSION: PLANET FORMATION (Planetesimals) / DISKS (Modelling) The formation of kilometer-sized planetary building bricks, called planetesimals, is still a hotly debated problem. However a quantitative model on when and where what sizes of planetesimals do form is the key to any self consistent formation model for gas giants as well a terrestrial planets. A pure hit and stick model of dust grains faces several adversaries: from drift barrier, to bouncing and fragmentation barrier to finally the 10km barrier. Thus, models have been invoked that lead swiftly to 100km sized planetesimals from centimeter sized objects via turbulent concentration and gravitational collapse. In this talk I will highlight the role of zonal flows in magneto-hydrodynamical (MHD) active regions of the disk and vortices in the MHD-dead zones. In the latter radial and vertical stratification are the key of understanding the hydro-dynamical stability of these disks. The fact that these features are able to scratch the tiniest amount of small dust together in an amount sufficient, to trigger a streaming and gravitational instability enables us to work on a size distribution for initial planetesimals that resembles observational findings in the asteroid and Kuiper belt. 16.Willy Kley Circumbinary Planets: Their properties and formation SESSION: PLANET FORMATION / DISKS (Modelling) Circumbinary planets form a special subclass of exoplanets where the planets orbit around a central binary star. Due to the presence of a secondary, the circumbinary discs are dynamically excited and the planet formation process is made more difficult than around single stars. Additionally, their subsequent evolution is influenced by the disc dynamics. In the talk I will summarize the observational properties of circumbinary planets and will present recent results in modelling such systems. 17. Hiroshi Kobayashi Importance of collisional fragmentation in planet formation SESSION: PLANET FORMATION / DISKS (Modelling) Runaway and oligarchic growth produces a large planetary embryo in each annulus of a protoplanetary disk. Planetesimals stirred by large embryos have great random motions, resulting in collisional fragmentation between planetesimals. Further collisions between fragments grind them down until fragments of ~10m are removed by radial drift due to gas drag. As a result, the embryo growth is significantly stalled by collisional fragmentation. On the other hand, the collisional fragmentation might explain the size distribution of minor bodies in the Solar System and debris disks. I will discuss the formation condition for planets, asteroid belt, and debris disks, taking into account collisional fragmentation. 18. Eiichiro Kokubo The Basic Scaling Laws of Terrestrial Planet Formation SESSION: PLANET FORMATION (Embryos) The recent exoplanet surveys show that small close-in planets are more common than hot Jupiters in the Galaxy. Most of them are considered as terrestrial (rocky) planets. Thus it becomes increasingly important to generally understand the formation of terrestrial planets. In the standard scenario of terrestrial planet formation the final stage is the giant impact stage after the dispersal of a gas disk where protoplanets or planetary embryos formed by oligarchic growth collide with one another to complete planets. We have been investigating this stage by using N-body simulations. In the present paper, we review the basic scaling laws of terrestrial planet formation and discuss the formation of close-in super-Earth systems. 19. Alexander V. Krivov (only Friday) Debris Disks - First Lessons from Herschel SESSION: DISKS (Observations) Debris disks, belts of invisible planetesimals and their observable dust, are thought to be remnants of the planet formation process. These disks have been observed at far-infrared wavelengths in several large-scale and smaller programs of the Herschel Space Observatory. Herschel observations have revealed the presence of debris disks around at least 20% of stars across and post the main sequence, and increased the number of spatially resolved disks from about two dozens to approximately one hundred. Resolved images along with densely sampled SEDs allow one to more tightly constrain the properties of the disks. First statistical analyses of Herschel-resolved disks suggest a two-component structure (a Kuiper-like belt plus an asteroid-like belt) to be more common than a single-component architecture. The disk radii do not appear to correlate with the stellar luminosity, which might pose additional constraints on the planetesimal formation mechanisms. In-depth collisional modeling of a few selected bright, well-resolved disks uncovers some previously unexpected trends, too. The disks of A-type stars (e.g., Vega, beta Pic, HR 8799) are compatible with an active collisional cascade in a narrow, massive, Kuiper-like planetesimal belt with a pronounced inner gap and a broad dust halo extending outward. In contrast, the disks of solar-type stars (q1 Eri, HD 207129, HIP 17439) show sharper outer edges and an additional emission closer to the star. This emission can be equally well explained by inward drag of dust inward from a single narrow planetesimal belt, dust production across an extended planetesimal disk, and an additional inner disk. In all cases, the models suggest low dynamical excitation of the main belt, i.e. disks that are collisionally quiescent rather than active. It remains unclear, however, which mechanism is actually at work in these systems. Nor is it clear what causes the difference between the disks of earlier- and later-type stars, and to what extent possible planets in the disks are responsible for the observed disk properties. 20.Luigi Mancini Photometric follow-ups of transiting exoplanets with ground-based medium-class telescopes SESSION: EXO-PLANETS (Detections) It is now well ascertained that those extrasolar planets that transit in front to their parent stars deserve extensive follow-up observations because they are the only ones for which we can directly measure all their physical parameters. These information currently provide the best route to constructing the mass-radius diagram of exoplanets, which channels the theoretical formation/evolution models in the right path. However, many of the discovered transiting planets do not have high-quality light curves, so their physical properties are poorly known. In this perspective, we are leading a large program to obtain ultra-high-precision photometry of transit events, which are analyzed to accurately measure the physical properties of know planetary systems. Besides measuring and refining the physical properties of the planets and their parent stars, we also try to obtain additional information from the light curves, by identifying particular features of the systems (e.g. stellar activity) and investigating the composition of the planetary atmospheres by transmission photometry. In my contribution, I will present several observational strategies that we adopt to achieve these goals. 21.Yamila Miguel Hot rocky to gas planets: How host stars and realistic UV flux change the detectable features for Mini-Neptunes and rocky atmospheres SESSION: EXO-PLANETS (Atmospheres) Recent ground and space surveys resulted in the detection of many hot extrasolar planets. These planets are interesting targets for current and future observations, therefore, addressing their atmospheric structure and composition is a major issue and the aim of my work. For the hot potentially rocky exoplanets with an outgassed atmosphere we developed a simple approach to find their atmospheric composition according to their observable data (radius, semi-major axis and stellar effective temperature). For hot mini-Neptune and giant planets's atmospheres, we calculated an atmospheric grid that links astrophysical observable parameters - orbital distance and stellar type - with the atmospheric species expected in exoplanet atmospheres. We link a 1D code that calculates the atmospheric thermal structure with a photochemical model that includes disequilibrium chemistry and explore the effect of empirical model parameters on the results, for planets around a wide range of stellar types from F to M, including the effect of high FUV radiation on their atmospheres. Our results can be applied to current and future observations to characterize exoplanet atmospheres and serves as a reference to interpret atmospheric retrieval analysis results. 22. Mordasini Christoph Connecting microphysics during formation with exoplanet observations: the impact of grain opacity in atmospheres of protoplanets SESSION: PLANET FORMATION (Embryos) The number of extrasolar planet with an accurately measured mass and radius has recently increased very rapidly. This has allowed to constrain for the first time observationally the hydrogen/helium fraction as a function of a planet's mass. This relation is of high interest for planet formation theory: it allows to constrain the mechanisms that govern gas accretion during formation. A key quantity controlling gas accretion is the opacity due to tiny dust grains suspended in the atmosphere of protoplanets. If it is high, only tiny primordial H/He envelopes can be accreted. In the opposite case, already low-mass cores can accrete much H/ He. In this talk I will present a newly developed analytical model for the grain opacity. It predicts very low grain opacities. I will then shown the population wide consequences of different magnitudes of the grain opacity. Low grain opacities lead to gas-rich low-mass low-density planets, not unlike the ones detected in large numbers by the Kepler satellite. I will show that the observed mass-radius relationship indeed also points to low grain opacities in protoplanetary atmospheres. The consequences for giant plant formation are discussed as well as for the transition from solid to gas-rich low-mass planets. 24.Makiko Nagasawa Outcomes of planet-planet scattering SESSION: PLANET-FORMATION (Embryos) Planet-planet scattering is one of the mechanisms to explain relatively large eccentricities of observed exojupiters. Typical fates of orbital instability of the three planet systems are ejections of a planet, planet-planet collisions, and planet-star collisions. Our group performed numerical simulations of planet- planet scatterings including tidal effects and showed a close encounter of a gas giant and a star can cause a hot-jupiter and the close encounter of gas giants can form binary planets. We will show the detailed results of numerical simulations of planet-planet scattering and discuss about their implications for future observations. 25.Taishi Nakamoto, Formation of solid materials in evolving solar nebula SESSION: PLANET-FORMATION (Planetesimals) We discuss the formation and evolution of solid materials seen in solar system bodies such as CAIs, chondrules, chondritic matrix, etc. These materials are thought to be formed in solar nebula, thus we discuss their formation in the solar nebula taking into account the formation and evolution of the solar nebula itself. In addition, we discuss a possible scenario of the agglomeration of dust particles, the formation of planetesimals, and the growth of protoplanets, in the context of the solid materials formation and evolution. 26. Hideko Nomura Complex Organic Molecules in Protoplanetary Disks SESSION: DISKS (Observations) We investigate the synthesis of complex organic molecules (COMs) in protoplanetary disks using a large gas-grain chemical network including COMs together with a 2D steady-state physical model of a disk irradiated by UV and X- rays from the central star. We find COMs are efficiently formed on cold and warm grains in the disk midplane via grain-surface reactions through efficient migration of icy species on grain surface. Radiation processing on ice forms reactive radicals and helps build further complexity. Part of the icy molecules are photodesorbed into gas and their transition lines become observable. We also perform ray-tracing calculations to predict line spectra of complex organic molecules and suggest CH3OH should be readily observable in nearby protoplanetary disks with ALMA. We also find the grain-surface abundances predicted by our calculations are consistent with those derived from cometary comae observations providing an evidence for the hypothesis that comets and other planetesimals formed via the coagulation of icy grains in the Sun's natal disk. 27.Satoshi Okuzumi Electric-field heating of plasmas and its effect on magnetorotational turbulence in protoplanetary disks SESSION: PLANET FORMATION / DISK (Modelling) The electric conductivity of the gas is a key parameter of magnetohydrodynamics (MHD) in low-temperature astronomical objects like protoplanetary disks. It is commonly assumed that the conductivity is independent of the strength of the electric field (as measured in the neutral-gas rest frame), and this assumption leads to the conventional linear Ohm's law. However, the linear Ohm's law breaks down when the electric field is so strong that heating of plasma particles is non- negligible. In fact, an order-of-magnitude estimate based on the results of recent MHD simulations suggests that the plasma heating is indeed significant in MRI- driven turbulence in some outer parts of protoplanetary disks. We construct a charge reaction model that takes into account plasma heating by electric fields as well as plasma capture by dust grains. We find that plasma heating leads to a reduction of the ionization degree, and hence to an enhancement of the magnetic resistivity, unless the electric-field strength is below the discharge threashold. This occurs because the electron--grain collision frequency increasing with increasing the random velocity of electrons. This effect may limit the saturatation amplitude of MRI-driven turbulence near the outer edge of the conventional dead zone. 28. Andreas Quirrenbach, CARMENES Consortium CARMENES: Searching for Blue Planets Orbiting Red Dwarfs SESSION: EXO-PLANETS (Detection) CARMENES (Calar Alto high-Resolution search for M dwarfs with Exo-earths with Near-infrared and opti-cal Echelle Spectrographs) is a next-generation instrument currently under construction for the 3.5m tele-scope at the Calar Alto Observatory by a consortium of eleven Spanish and German institutions (see also Quirrenbach et al. 2010; 2012). CARMENES will conduct a 600-night exoplanet survey targeting ~300 M dwarfs. An important and unique feature of the CARMENES instrument is that it consists of two separate échelle spectrographs, which together cover the wavelength range from 0.55 to 1.7 μm at a spectral resolu-tion of R = 82,000. The spectrographs are fed by fibers from the Cassegrain focus of the telescope. For late-M spectral types, the wavelength range around 1.0 μm (Y band) is the most important wavelength region for radial velocity work. Therefore, the efficiency of CARMENES will be optimized in this range. The main scientific objective of the CARMENES project is to carry out a survey of late-type main sequence stars with the goal of detecting low-mass planets in their habitable zones (HZs). In the focus of the project are very cool stars later than spectral type M4 and moderately active stars. In particular, we aim at being able to detect a 2M⊕ planet in the HZ of an M5 star. A long-term radial velocity precision of 1ms−1 per measure-ment will permit to attain such goals. For stars later than M4 (M < 0.25M⊙), such precision will yield detec-tions of super-Earths of 5M⊕ and smaller inside the entire width of the HZ. The CARMENES survey will thus provide a comprehensive overview of planetary systems around nearby Northern M dwarfs. By reaching into the realm of Earth-like planets, it will provide a treasure trove for follow-up studies probing their habitability. 29.Sabine Reffert Giant Planet Occurrence Rate as a Function of Stellar Mass and Metallicity SESSION: EXO-PLANETS (Detection) Based on our precise Doppler survey of a sample of G and K giant stars, which we have carried out at Lick Observatory over more than 12 years, we examine the planet occurrence rate as a function of stellar mass and metallicity. In particular, we probe the stellar mass range from about 1 to 3 solar masses, which is neither being fully explored by main-sequence nor subgiant stellar samples. We find the well-known planet-metallicity correlation, as well as a strong dependence of planet occurrence on stellar mass. Interestingly, there is a peak in the giant planet occurrence rate for masses between about 1.5 and 2.0 solar masses. For masses in the range from 2.5 to 3.0 solar masses, the giant planet occurrence rate drops rapidly to zero, at least for those giant planets to which our survey is sensitive. We conclude that giant planet formation is suppressed around higher mass stars, possibly due to faster disk depletion in combination with a longer migration timescale. 30. Semenov Dimitry Importance of dynamical processes for chemical evolution of protoplanetary disks SESSION: DISKS (modelling) Protoplanetary disks are birth sites of planetary systems. A better characterization of their physical and chemical structure, which are needed to understand initial phases of planet formation, is currently one the major goals of modern astrophysics. Their studies are complicated by their compact sizes and low masses, and their dynamical activity. In this presentation we investigate the importance of dynamics on the chemical structure of disk's gas and dust. We find that dynamics enhances abundances of many gas-phase species and ices, particularly, complex hydrocarbons involved in slow X-ray-driven CO destruction. Particularly affected by dynamics are the inner, planet-forming disk regions, with strong gradients of temperature and high-energy radiation intensities. We show how evolving chemistry affects the global C/O gas and solid composition and why it may matter for planet formation processes. 31.Takanori Sasaki Re-entry of giant-impact fragments and early evolution of the Earth. SESSION: PLANET FORMATION (embryos) The late stages of Earth’s formation remain a mystery. No building blocks remain in Earth’s orbit and no geological evidence is available for the first 700 million years Earth’s history. Clues have been found, but some of them seem paradoxical. Herein we propose that protoplanetary fragments produced by the giant impacts may reconcile those apparently conflicting facts. Our new scenario present an exhaustive framework of early evolution of terrestrial planets, and impact our understanding of whether planets like Earth are common in extrasolar systems as well. I’m looking forward to discussing with German researchers at the meeting 32.Takayuki Muto Protoplanetary Disk Morphology and High-Resolution Imaging Observations SESSION: DISKS (Observations) Understanding protoplanetary disks is important in understanding planet formation processes. Recent observations by Subaru and ALMA have revealed that protoplanetary disks are rich in detailed structures, and the gas and dust are distributed differently. We present results of recent observations by ALMA and Subaru and modeling efforts of protoplanetary disks. We especially focus on non-axisymmetric structures such as spirals or horse-shoe-like dust condensations, and discuss what we can derive from such structures. We also mention about prospects of future high-resolution imaging observations by 30- meter class telescopes or full ALMA capability. 33. Taku Takeuchi Transport of the Magnetic Flux in Protoplanetary Disks and Disk Evolution via MHD Turbulence and/or Winds SESSION: PLANET FORMATION / DISKS (Modelling) I present our recent works on the transport of the magnetic flux which is originally from the interstellar magnetic field and threads the disk. Then, I discuss disk evolution that is controlled by the magnetic flux via MHD turbulence and/or winds. Recent several MHD simulations have suggested that the mass accretion rate driven by the MRI or disk winds is controlled by the magnetic flux threading the disk. This means that quantifying the magnetic flux is essential for studies on the disk accretion. We analyzed a simple model of the mean poloidal field in a thin disk. We show that there is an upper limit on the magnetic flux threading the disk, and consequently there is also an upper limit on the mass accretion rate. I also discuss the evolution of protoplanetary disks whose accretion rates are determined by the magnetic flux. An interest finding is that, contrary to previous expectations, dead zones do not always suppress the mass accretion rate. Even in an inner part where a dead zone exists, if the magnetic flux is high enough, the mass accretion rate can be as high as or even higher than that at the outer active region. Such stronger accretion at the inner part is expected especially at late stages of disk evolution. This mechanism possibly explains an inner hole of some transitional disks. 34. Hidekazu Tanaka Fluffy Dust Growth and Planetesimal Formation SESSION: PLANET FORMATION (Planetesimals) Planetesimal formation is one of the major problems in planet formation theory. Rapid direct growth of fluffy icy dust is a hopeful model for planetesimal formation. In this model, the key point is the mechanical property of dust aggregates (i.e., their stickiness and compressibility). I will talk about recent progress on dust aggregate simulations in our group and discuss planet formation, too. 35. Motohide Tamura Subaru Direct Imaging Observations of Exoplanets and Brown Dwarfs SESSION: EXO-PLANETS (Detection) SEEDS (Strategic Explorations of Exoplanets and Disks with Subaru) is the first Subaru Strategic Program, whose aim is to conduct a direct imaging survey for giant planets as well as protoplanetary/debris disks at a few to a few tens of AU region around 500 nearby solar-type or more massive young stars devoting 120 Subaru nights for 5 years. The targets are composed of five categories spanning the ages of ~1 Myr to ~1 Gyr. Some radial velocity planet targets with older ages are also observed. The survey employs the new high-contrast instrument HiCIAO, a successor of the previous NIR coronagraph camera CIAO for the Subaru Telescope. We describe the outline of this survey and present its results on exoplanets and brown dwarfs. The survey has published ~30 refereed papers by now. The main results on exoplanets are as follows: (1) Detection and characterization of the most unequivocal and possible lowest-mass planet around the Sun-like star, GJ 504b, via direct imaging. It is so far the only exoplanet whose atmospheric methane features make their color “blue” among the other directly imaged “red”-color exoplanets. (2) Detection of a super-Jupiter around the most massive star ever imaged, kappa And b. (3) Detection of planet or brown dwarf around Sun-like star, GJ 758b, and several brown dwarfs in Pleiades. (4) Detection of companions around retrograde exoplanet, HAT-P-7B, which supports the Kozai mechanism for the origin of retrograde orbit. Preliminary statistics in each category are also mentioned. 36. Mario Trieloff Compositional variety among planets: When and how were compositional gradients established in the early solar system? SESSION: PLANET FORMATION (Planetesimals) Our solar system is clearly divided in rocky planetary bodies in the inner solar system, and gas and ice giants planets in the outer solar system. While this roughly corresponds to expectations from condensation temperatures prevailing in the solar nebula, governed by the protosun and protoplanetary disc dynamics, many details concerning the compositional diversity of solar system objects are unknown, even after decades of research in cosmochemistry. One important question is how homogeneous the initial disk material was, particularly the dust component inherited from the interstellar medium (ISM). While certain interstellar grains definitely represent isotopically anomalous circumstellar dust, it is not clear, what their mass fraction in the ISM is, and what fraction was homogenised in the ISM by evaporation and recondensation processes. However, even if highly heterogeneous grain populations dominated the solar nebula, large scale mixing of submicron sized interstellar grains should have cancelled out large scale chemical heterogeneities. Indeed we know that certain primitive extraterrestrial matter represented by CI chondrites represent a first order average composition of solar or cosmic element abundances. On the other hand, there are chondrite classes that are characterised by 1) moderately volatile element depletions 2) intra-silicate (olivine/pyroxene) fractionation 3) metal-silicate fractionation which is generally interpreted as being a result of (mainly thermal) processing in the solar nebula, along with gas-solid phase separation before planet formation started. While such fractionation processes within a protoplanetary disc are feasible, there are mixing processes simultaneously at work, which should counteract differentiation. For example, mixing processes are evident from the presence of high temperature material such as CAIs or refractory forsterites in cometary material, implying radial transport form hot inner to the cold outer disk regions. The composition of volatile-rich exoplanets is frequently explained by planetary migration processes, implying that their material could not have accreted in their present day's orbital position. Such conclusions can only be properly established, if the chemical (and isotopic) compositon of protoplanetary material in the respective feeding zones can be modelled by means of (chemical) disc fractionation and counteracting radial mixing processes at the preplanetary stage. 37.Roy van Boekel The link between planet formation and planet atmosphere spectra SESSION: EXO-PLANETS (Atmospheres) The composition of a planet and its atmosphere are governed by its formation history in the circumstellar disk and its further evolution. During the early formation phase a rocky core is formed, which may subsequently accrete a gaseous envelope once the core mass succeeds a critical value, forming a giant planet. While Hydrogen and Helium dominate the mass of the envelope and atmosphere of giant planets, their spectral appearance is dominated by the abundance of heavy elements needed to build spectroscopically active molecules (e.g. water, methane). The molecular composition of mature exoplanet atmospheres depends on the relative abundances of heavy elements in the envelope, which follow from the accretion history during the formation phase. In this talk we will present model calculations of the formation of giant planets, following which kind of material is accreted depending on the formation location in the disk. We will focus on the circumstances under which an oxygen-rich or a carbon-rich chemistry results. We also show the resulting atmospheric spectra of mature planets, and simulated observations of transiting systems with which the discussed cases can be distinguished.” 38. Joachim Wambsganss Searching for Extrasolar Planets with Gravitational Microlensing: Challenges and Exciting Results SESSION: EXOPLANETS (Detection) Gravitational microlensing is a powerful method for the detection of extrasolar planets. In particular its sensitivity to low mass planets and its potential for global statistical analyses are highly relevant. The basics of this technique and its current mode of operation will be explained as well as its advantages and disadvantages compared to other planet-search methods. About three dozen microlensing planets have been discovered so far. A couple of microlensing detections will be presented and reviewed in detail. A recent statistical analysis on the Galactic abundance of extrasolar planets will be presented and discussed, with particular emphasis on the result that “Planets are the rule, not the exception ”. In a brief outlook, the immense potential of gravitational microlensing for detections of Earth- and Mars-mass planets, of exomoons and of free-floating planets will be highlighted. 39.Sebastian Wolf High-angular resolution observations and modeling of circumstellar disks SESSION: DISKS (Observation) Observations of circumstellar disks around young stars are the key to better understand and to refine existing hypotheses for the various phases of the planet formation process. I will present modeling approaches based on observations in various wavelength ranges at low to high spatial resolution. Exemplary case studies will be discussed which illustrate state-of-the-art observations and subsequent radiative transfer modeling of protoplanetary and debris disks. 40. Wurm Gerhard Collisions of Small Bodies in Protoplanetary Disks: Cold, Hot, and Viscous SESSION: PLANET FORMATION (Planesimals) The physics of silicate collisions at moderate temperatures has been treated extensively in the past decades showing the potential and limits in planetesimal formation. The microphysics of more extreme environments with high and low temperature has mostly been restricted to numerical modeling and only recently emerges in experiments. We currently exploit some aspects here. We measure ice contact forces for nm to µm grains, study the evolution of contact forces and collisions with increasing temperatures toward 1000 K, and study collisions of viscous particles as chondrule analogs. I will sketch our latest evolution on these topics