This is not a blog post as such, it’s the notes that I took during the conference split up into sections. Unfortunately there is no reference to the talk content itself; this is kept in the booklet which I have sitting next to me as I type this.

Session 1

Detecting and characterising via direct imaging

• More than 2Gyr gas giants more than 10^8 times fainter than primary
• Young stars are 10^4 - 10^7 times better than this
• Chronograph for increasing contrast
• Speckle noise a big problem
  • for speckle based data S/N does not increase with time
  • angular differential imaging
    • speckles oscillate while image rotates, but keep similar shape
    • real objects will move in the frame
• A stars good targets despite being bright
  • higher hosting fraction for giant planets for A stars (not sure about this)
  • high profile detections
  • Nielsen show low host fraction despite this
• M stars also good targets
  • despite low independent host fraction
• Typical contrasts - 10^5 at 1 arcsecond (with NICI)

Physical properties (atmospheres)

• Direct photons detected from these objects
  • reflected light and background contaminants surely?
• Colours in infra-red shows deviations from the predicted T dwarf type sequence (brightness vs colour)
  • more like L dwarfs
  • much lower surface gravity
• Direct spectra taken (!)
• Huge spectral diversity for planets even in same system
• Surface gravity strongly affecting the spectra
• Orbits of Beta Pic 2 - Chauvin et al. 2012
  • most probable semi major axis

Architecture

• Upper limits to abundance
• Cold start - less than 10% for separations 20 - 630 AU
• Hot start - less than 10% for separations 10 - 810 AU
• Gravitational instability planets rare at more than 10 AU
• Scattering planets also rare
• Sphere project - 10 - 80 more planets
• Possible detection of Super-Earth around nearby M dwarf (Crossfield, Goyon et al. 2013)

Summary

• Young exoplanets have red colours consistent with dusty clouds and non-equilibrium chemistry
• Hot start gas giant planets more than 4 MJup rare at more than 10AU

International deep planet survey

• Homogeneous analysis methods

SEEDS

• Strategic Explorations of Exoplanets and discs with Subaru
• Variety in morphology of protoplanetary discs
  • gaps, non-uniform shapes
• IRD - IR doppler instrument on Subaru
  • could be good for follow up for NGTS, investigate this
  • paper

Hershell dust evolution in discs

• SED modelling and Herschel tracing dust evolution in discs

###Planet formation in evolving protoplanetary discs

• Gas dominates planetary formation
• Planets form in evolving discs
• Disc dispersal quick and efficient
  • relatively few systems found with partial discs
• Accretion in disc core, with photoevaporation at higher disc heights
• Changes in disc structure can form traps for dust or planets
• Final gas disc dispersal halts planet migration
• Giant planet migration can be halted if the disc gas is dispersed
• RDA & Armitage 2009, RDA and Pascucci 2012
• Pile up observed in models and data at 1-2AU
  • looks like a possible pile up at smaller separations also

Disc inhomogeneities and the origins of planetary system architectures and observational properties

• Discs have 3 types of planet trap

HST/STIS imaging of Fomaulhaut: New main belt structure and confirmation of Fomalhaut b’s eccentric orbit

• Highly eccentric 0.8
• A ~= 1.77
• Periastron: 32AU
• P ~= 1700 years
• Dynamically linked with belt
  • mutual inclination (planet - belt) ~ 17 degrees
  • Periastron linked
• Gap in main belt of ~50AU
• Inner belt detected
• Planet planet scattering: Chatterjee et al. 2008

Highlights of Exoplanet Characterization

• Planets are diverse in Teff(planet) vs IR colour, no clear pattern yet
• Uranus and Neptune heavily enriched in carbon (50x)
  • also very old, about 50K
• Consistent non-detection of CO in GJ436
• Featureless atmosphere of GJ1214b suggests high mean molecular weight
  • dramatic cloud obscuration
  • high water constituent
• Low mass planets may have high Zenv (metal fraction of the envelope)
• GJ3470b - Uranus analogue
• GJ436b has dayside and transit data breaking atmospheric degeneracy
• Comparisons of C/O ratio for star and planet v. interesting

Planets around low mass stars (PALMS) high contrast imaging survey

• Link with microlensing
• Snapshot program - breadth not width
• Gravity-dependant L to T dwarf transition

Session 2

Review

• Radio maps more than 95% of mass
  • good for structure

Triggered planet formation in action: resolved gas and dust images of a transitional disk and its activity

• Surface density excess after a planetary body traps large dust particles in a potential maximum
• Increased density leads to planet formation

Session 3

Review - The story of planets: anchoring numerics to reality

• Hubble protoplanetary disk atlas - nice pictures
• Disc gaps depend on grain size - different wavelengths probe grain size and gap width
• Grain growth drives planetessimal (~km sized) formation
  • not reliable
• Pairwise accretion - slow, turbulence high, has issues
  • requires velocity dispersion/distribution in simulations
    • mean velocity is not enough for an accurate simulation
  • requires grain size distribution
• Pressure bumps trap dust
  • leads to further processes, gravitational instability, accretion
• Accretion very low fraction of simulated collisions
• Dust distribution dependant on planetessimal eccentricity

Zooming in on protoplanetary discs

• Magnetic fields in star forming region does not create planar disc initially
  • vertical structure is created
• Free-fall accretion guided by magnetic field

Planetessimal formation

• Disc cross section
  • core stable
  • edges suffer instability
• Planet trend with instability
  • mostly requires local Disk metalicity, could be super-solar

Session 5

A decade and a half of AngloAustralian Planet Searching

• 240 stars sample over 15 years
• 2.5 meters per second precision
• HD 20782 - highest eccentricity 0.952
• Wittenmyer et al., 2011, apj - reference for false rv signal testing
• R ~ 60000 - S/N needs to be 5000
• FunnelWeb - spectra of all stars V less than 12, delta less than 20, 390-800nm Very nice talk

The Debiased Kuiper Belt: Our Solar System as a Debris disc

• 20% large KBOs more than 100km are in resonance with Neptune

Planets and Stellar Activity: Hide and Seek in the CoRoT-7 system

• Active granulation effects for RV
  • bright blue cells dominate cool red cells = net blueshift
  • creates RV signal of ~ 1m/s
• Use lightcurve without transits to provide activity profile
  • simultaneous observations
  • RV profile then contains both stellar noise and planet
  • use lightcurve as basis function

Properties of the young gas giant planet Beta Pictoris b

• Planet on inclined orbit around star, inclined wrt disc

Characterizing the Demographics of Exoplanet Bulk Compositions

• New kepler mass radius relations with Keck

Unveiling an exoplanetary Neptunian atmosphere through multiband transit photometry

• Infra-red used to measure bands H2O, CO, CH4

The Shocking Variability of Exoplanet Transits

• WASP-12 b bow shock in the infra-red

Session 6

Debris discs as components of extrasolar planetary systems

• Debris disc descendant of protoplanetary disc

• Proplyds

  • less than 10MYr
  • optically thick
  • more than 10 Mearth
  • ~100x dust mass
  • dust from 0.1-100AU
  • primordial?

• Debris

  • 10MYr -10Gyr
  • optically thin
  • less than 1 MEarth
  • no gas
  • ~30AU ring

• Inner holes caused by planets?

• Inner edge of disc predicted to be carved by planets

  • shape of the edge depicted by planet mass

• CO short lifetime ~100 years due to photo-disassociation

• Clump in disc

  • could be through planet orbit and gravitaitonal influence
  • could be a destruction event causing debris to pass through the same point leading to higher density

• Alma probes mm sized dust - traces planetessimals

• Scattered light probes micron sized dust

• Systems with planets are brighter (SKARPS, Herschel) than systems without implying debris discs

A Resolved Millimeter Emission Belt in the AU Mic Debris disc

• Best fit model suggests increasing surface density with radial distance
  • inner collision depletion?

Detailed model of the exozodiacal disc of Fomalhaut and its origin

Final Results of the Herschel Open Time Key Programme DUNES

• 16 resolved discs, 13 new

Session 7

Review

• Morbidelli+ 2009, planetessimal simulation
• Rafikov 2004, proposed explanation of accelerated core accretion
  • neptune in less than 10Myr

Rapid growth of giant planet cores by pebble accretion

• Pebble accretion can rapidly grow the planet mass and deal with collapse, according to the model
• Author: Lambrechts

Planet Formation and Evolution in Traps: Origins of the MassPeriod Relation

• Traps catch planets while forming
• Rapid envelope accretion process
• Model predicts that super earths are failed jovian cores
• Putdritz model looks interesting
  • predictions for hot Jupiter formation
• Giant planets start at greater than 0.7Msolar

Session 8 - evolution of planetary systems

Review

• Interesting deficit of period ratios in Kepler dataset just below 2:1
• Resonances cause oscillations of the periastron points of a multiple system
  • non-resonances cause circulation
• If the system is not stable with aligned systems (angle of periastrons equal) then all other configurations will be unstable
• No close encounter required
• Hill radius associated with circular orbits
• Dissipation acts to stabilise systems
• HAT-P-13 is multiple planet system
  • why does WASP not find any?
  • consider changing wasp pipeline to subtract the in-transit data and re-perform search N times
• MMR Lithwick
• Could the Kepler distance from pure resonances be due to unseen non-transiting bodies?

Constraining planetary migration mechanisms in systems of giant planets

• Dawson and Johnson 2012 - predicting eccentricity from Kepler lightcurves
• Metal-poor and metal-rich lead to disk migration
  • only metal rich stars form multiple systems
• Fressin et al. 2013 - kepler occurrence rates
• Possible pile up at short periods for metal rich Kepler host stars
• How do eccentric planets in the period valley between 0.1 and 1 AU form?
• Planet planet scattering possibly ejecting outer planet removing it from evidence for it

The Impact of Stellar Multiplicity on Planetary Systems

• High protoplanetary disc occurrence for wide binary planets
  • distinct decrease below binary star separations of ~40AU
• Similarly decreasing disc mass with decreasing orbital separation
• RV surveys biased against binary stars due to the stray light from the binary companion in the slit
• Only equal flux binaries at short separations
  • selection effect?
    • maybe planets form around the fainter secondary and are therefore harder to detect so we don’t find them

Orbital structure of Kepler Planetary Systems

• Low mass planets targeted for the talk
  • less than ~30Mearth
• Fortney 07 density structures
• Bimodal small radius distribution
  • can be split by the x-ray exposure
• TTV mass estimations extremely sensitive to eccentricity

Archaeology of Exo-Terrestrial Planetary Systems

• RECONS project - spectral types within 10pc