the influence of planets on disk observations (and the influence of disks on planet observations)
DESCRIPTION
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. - PowerPoint PPT PresentationTRANSCRIPT
The Influence of Planetson Disk Observations
(and the influence of diskson planet observations)
Geoff Bryden (JPL)Doug Lin (UCSC)Hal Yorke (JPL)
G. Bryden (JPL) Effect of Planets on Disk Observations
What kind of disk features should we expect?
• Planetary Gaps
• Spiral Waves
• Accretional Hot Spots
• Shadowed Regions
• Large Inner Holes?
G. Bryden (JPL) Effect of Planets on Disk Observations
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.
G. Bryden (JPL) Effect of Planets on Disk Observations
Model Parameters
G. Bryden (JPL) Effect of Planets on Disk Observations
Axisymmetric Disk (no planet)
T
ρ
G. Bryden (JPL) Effect of Planets on Disk Observations
Axisymmetric Disk (no planet)
T
ρ
G. Bryden (JPL) Effect of Planets on Disk Observations
Axisymmetric Disk (no planet)
T
ρ
G. Bryden (JPL) Effect of Planets on Disk Observations
Temperature v.s. Radius
Midplane Temp.
(ChiangGoldreich power-law)
Surface Temp.
G. Bryden (JPL) Effect of Planets on Disk Observations
Gap-Opening, Jupiter-Mass Planet(side view)
T
ρ
G. Bryden (JPL) Effect of Planets on Disk Observations
Temperature v.s. Radius:with/without a gap
Gap
No Gap
G. Bryden (JPL) Effect of Planets on Disk Observations
Spectral Energy Distributions
SED components
with/without a gap
v.s. Inclination
G. Bryden (JPL) Effect of Planets on Disk Observations
Observing Gap Formation with ALMA
Wolf et al. 2002
4 hour integration on ALMA
• Jupiter-mass planet at 5.2 AU• 0.7mm images
G. Bryden (JPL) Effect of Planets on Disk Observations
Embedded, Neptune-Mass Planet(side view)
T
ρ
G. Bryden (JPL) Effect of Planets on Disk Observations
Embedded Planet:1AUx1AU View of the Fountain Flow
T
ρ
G. Bryden (JPL) Effect of Planets on Disk Observations
Space Interferometry Mission
SIM will attempt to detect the astrometric signal of young planets just as they are forming.
G. Bryden (JPL) Effect of Planets on Disk Observations
Sources of Astrometric Wobble
1. Planet’s Gravitational Pull
2. Disk’s Gravitational Pull
3. Disk’s Photospheric Signal (center-of-light wobble)
G. Bryden (JPL) Effect of Planets on Disk Observations
Rotating Gap-Opening Planet
G. Bryden (JPL) Effect of Planets on Disk Observations
Rotating Embedded Planet
G. Bryden (JPL) Effect of Planets on Disk Observations
Inner Disk Holes
Inner holes may be caused by:• Photoevaporation (Clarke)• Giant planet torques (Wood)• Dust coagulation• Planet accretion • Misinterpreted SED (Boss & Yorke 1996)
G. Bryden (JPL) Effect of Planets on Disk Observations
SEDs for Disks with Inner Holes
R_in = 0.05 AU
R_in = 100 AU
G. Bryden (JPL) Effect of Planets on Disk Observations
Spitzer IRAC color excessesv.s. Inner Hole Size
G. Bryden (JPL) Effect of Planets on Disk Observations
Summary(yes, this is the last slide, so pay attention now)
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.
ALMA should easily detect protoplanetary gaps for Jupiter-like planets. Evidence of embedded proto-Jupiters (hotspots/extended shadows) is much more difficult.
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.