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01Dec2006 The Big Picture Ge/Ay133 Review/ 0.05-5 AU region. - - PDF document
01Dec2006 The Big Picture Ge/Ay133 Review/ 0.05-5 AU region. - - PDF document
01Dec2006 The Big Picture Ge/Ay133 Review/ 0.05-5 AU region. Jovian planets througout the And No strong preference for orbital distances except for a pile up of hot Jupiters at P~3 days. Why do we care about gas
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No strong preference for orbital distances… …except for a “pile up” of hot Jupiters at P~3 days.
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Disk-star- and protoplanet interactions lead to migration while the gas is
- present. Core-
accretion & ice?
Why do we care about gas & ice in disks? Theory Observation?
1 AU at 140 pc subtends 0."007. Jupiter (5 AU): Vdoppler = 13 m/s Vorbit = 13 km/s
Simulation G. Bryden (JPL)
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Characterizing large disk samples? SED Models:
IR disk surface within several 0.1 – several tens of AU (sub)mm disk surface at large radii, disk interior.
G.J. van Zadelhoff 2002 Chiang & Goldreich 1997
HH 30
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Statistically, how long do gas/dust rich disks “survive”? Basic result: Disks dissipate within a few Myr, but with a large disp. for any SINGLE
- system. When
they go, however, the dissipation is FAST in comparison w/ disk “lifetime.”
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Hollenbach et al. (2000, PP IV)
Putting it all together: A comparison of various disk dispersal mechanisms
The stellar encounter (SE) and external photo- evaporation time scales are calculated for the core of the Orion proto- stellar cluster.
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Did the Sun form as part of a rich cluster?
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terrestrial terrestrial One important set of clues: Short-lived nuclides in meteorites
Murchison Thin section (chondrules)
CAIs
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How do we tie astronomy & meteorite timescales together?
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How do disks evolve, REALLY?
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This? Or this? Turbulent disks & stochastic migration.
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Look at time to open a gap as compared to the viscous response time scale of the disk gas. Find: Planet mass needed to open gap:
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CO Good Dynamical, Temp. Tracer
- M. Simon et al.
2001, PdBI
The CO line shape is Sensitive to: Rdisk ,Mstar, Inc. These can be measured w/resolved images:
Dent et al. 2005, JCMT vLSR (km/s) TMB (K)
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Disk chemistry?
Depending on dust opacity, cores may spend a long time in the “plateau” phase before runaway gas accretion. Form cores closely spaced in higher density region.
Need spatially resolved measurements of disk gas & its composition.
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Enter ALMA:
Llano de Chajnantor; 5000 m, good for astronomy, tough for humans!
Superb site & large array exceptional performance (50 12m telescopes, by 2012).
Dust simulation (L.G. Mundy), realistic phase errors, but no CLEAN/MEM.
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When rings are seen around >10 Myr old stars… the dust must be made in place.
- CSO/HST have reached similar
conclusions about structure of the disk around Fomalhaut and how it is generated. Is there a planet required to maintain it?
Marsh et al. – ApJ, Feb. 2005 Kalas, Graham, & Clampin – HST, Nature, June 2005
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The future: discovery space for indirect methods…
Radial velocity Astrometry
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HD 149026
Transiting systems rare but incredibly informative…
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… and photometry from space can be extremely good!
HD 209458 - HST
Brown, T.M. et al. 2001, ApJ, 552, 699
The KEPLER mission is dedicated to photometry and can search for earth mass planets in the so- called habitable zone via transits.
www.kepler.arc.nasa.gov
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Comet dust assembled from sub- micron sized components. IDPs can be analyzed in the lab!
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Samples of known provenance!
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1999 KR 16
First (non-Pluto) trans-Neptunian
- bject found in
1992 (Jewitt & Luu), now many many hundreds. They are found through their motion on the sky, gives R,i fairly quickly.
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N e p t u n e c r
- s
s i n g 3:2 2:1 Plutinos classical KBOs scattered KBOs
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What can meteorites tell us about the early S.S.?
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These irons and pallasites likely originate in the cores
- r core-mantle boundaries
- f differentiated bodies.
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The atmosphere is also strongly affected by core formation, and its timing.
Equilibrium Gas Abundances in Silicate Magmas
SiO2 + 2Fe3O4 → 3Fe2SiO4 + 02 SiO2 + 2Fe + O2 → Fe2SiO4
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The future: discovery space for indirect methods…
Radial velocity Astrometry
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Finding other Earths? The Space Interferometry Mission (SIM)
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If we locate other Earths, how might we then characterize them in detail? TPF-C TPF-I
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Nulling: Use the fringes to suppress the central
- star. First
tests w/ Keck in 2006. TPF?...
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What can remote sensing of atmospheres tell us?
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What would be possible with TPF as presently envisioned? About R≈100 even in the very best set of circumstances. What might you want?
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Coupled evolution of the biosphere and atmosphere:
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