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The Influence of Planets on Disk Observations (and the influence of disks on planet observations)

The Influence of Planets on Disk Observations (and the influence of disks on planet observations). Geoff Bryden (JPL) Doug Lin (UCSC) Hal Yorke (JPL). What kind of disk features should we expect?. Planetary Gaps Spiral Waves. Accretional Hot Spots Shadowed Regions.

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The Influence of Planets on Disk Observations (and the influence of disks on planet observations)

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  1. The Influence of Planetson Disk Observations (and the influence of diskson planet observations) Geoff Bryden (JPL) Doug Lin (UCSC) Hal Yorke (JPL)

  2. What kind of disk features should we expect? • Planetary Gaps • Spiral Waves • Accretional Hot Spots • Shadowed Regions • Large Inner Holes?

  3. Computational Method Computational requirements: 1. hydrodynamics near the planet 2. radiative transfer throughout the disk 3. detailed consideration of the surface heating • Flux-limited diffusion with stellar ray tracing This radiative hydrodynamic method is ideal for following the feedback between disk structure and stellar irradiation.

  4. Model Parameters

  5. Axisymmetric Disk (no planet) T ρ

  6. Axisymmetric Disk (no planet) T ρ

  7. Axisymmetric Disk (no planet) T ρ

  8. Temperature v.s. Radius Midplane Temp. Surface Temp. (ChiangGoldreich power-law)

  9. Gap-Opening, Jupiter-Mass Planet(side view) T ρ

  10. Temperature v.s. Radius:with/without a gap No Gap Gap

  11. Spectral Energy Distributions SED components with/without a gap v.s. Inclination

  12. Observing Gap Formation with ALMA Wolf et al. 2002 • Jupiter-mass planet at 5.2 AU • 0.7mm images 4 hour integration on ALMA

  13. Embedded, Neptune-Mass Planet(side view) T ρ

  14. Embedded Planet:1AUx1AU View of the Fountain Flow T ρ

  15. Space Interferometry Mission SIM will attempt to detect the astrometric signal of young planets just as they are forming.

  16. Sources of Astrometric Wobble 1. Planet’s Gravitational Pull 2. Disk’s Gravitational Pull 3. Disk’s Photospheric Signal (center-of-light wobble)

  17. Rotating Gap-Opening Planet

  18. Rotating Embedded Planet

  19. Inner Disk Holes • Inner holes may be caused by: • Photoevaporation (Clarke) • Giant planet torques (Wood) • Dust coagulation • Planet accretion • Misinterpreted SED (Boss & Yorke 1996)

  20. SEDs for Disks with Inner Holes R_in = 0.05 AU R_in = 100 AU

  21. Spitzer IRAC color excessesv.s. Inner Hole Size

  22. Summary(yes, this is the last slide, so pay attention now) Spitzer observations (IRAC & IRS) can be used to characterize disks in the planet-forming region around young stars. In particular, inner disk holes will be identified in this region. ALMA should easily detect protoplanetary gaps for Jupiter-like planets. Evidence of embedded proto-Jupiters (hotspots/extended shadows) is much more difficult. SIM will be able to observe young planets, even when surrounded by a massive disk. This will address key questions such as: 1) where & when giant planets form, 2) how their eccentricity evolves, and 3) whether their distribution evolves with time.

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