The Formation

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The Formation Evolution of Planetary Systems
Placing Our Solar System in Context
Painting courtesy of William Hartman, Planetary
Science Institute, Tucson, AZ.

• Michael R. Meyer (Steward Observatory, The
  University of Arizona, P.I.)
• D. Backman (Franklin Marshall College, D.P.I.)
  , S.V.W. Beckwith (STScI), J.M. Carpenter
  (Caltech), M. Cohen (UC-Berkeley), T. Henning
  (Jena), L. Hillenbrand (Caltech, D.P.I.), D.
  Hines (Steward), D. Hollenbach (NASA-Ames), J.
  Lunine (LPL), R. Malhotra (LPL), P. Morris (SSC),
  J. Najita (NOAO), D. Padgett (SSC), D. Soderblom
  (STScI), J.R. Stauffer (SSC), S. Strom (NOAO),
  D. Watson (Rochester), S. Weidenschilling (PSI),
  and E. Young (Steward).
• 198th AAS Meeting, Pasadena, CA June 3-7, 2001

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The Formation and Evolution of Planetary Systems

• Circumstellar disks are the sites of planet
  formation.
• How does the gas and dust evolve in circumstellar
  disks surrounding solar-type stars?
• Where, when, and how frequently do planets form
  in circumstellar disks?
• Our ultimate goal is to characterize the
  diversity of planetary system architectures, in
  order to constrain the range of possible outcomes
  of the planet formation process - thereby
  placing our solar system in context.

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From Protostellar Disks to Mature Planetary
Systems
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Placing Our Solar System in Context with SIRTF

• First Mission of NASAs Origins Program
• 0.85 cm cooled space telescope in earth-trailing
  orbit
• Three Instruments IRAC, IRS, MIPS
• Five Year Lifetime with Science Goals including
  Galaxy formation evolution, Disks, Brown
  Dwarfs
• Additional Legacy Science Programs
• Dickenson et al. - Great Observatories Deep
  Survey
• Londsdale et al. - SIRTF Wide-field IR Survey
• Kennicut et al. - Star-formation in nearby
  galaxies
• Churchwell et al. - Galactic Planet Survey
• Evans et al. - Galactic star formation
• To learn more please visit http//sirtf.caltech.ed
  u

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Evolution of inner accretion disks as traced by
near-IR excess (Hillenbrand Meyer, in
preparation).
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Evolution of outer disks (0.3-3.0 A.U.) around
solar-type stars. IRAS data (s) should be
considered lower-limits in comparison to ISO data
(l) which are x5 more sensitive.
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SIRTF Legacy Science The Formation and
Evolution of Planetary Systems

• Formation of Planetary Embryos
• characterize transition from primordial to debris
  disks.
• Growth of Gas Giant Planets
• constrain timescale of gas disk dissipation.
• Mature Solar System Evolution
• examine the diversity of planetary systems.
• Our program builds on the heritage of
  IRAS and ISO.

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Evolution of Dust Mass in Small Grains
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Tracing the Evolution of the Gas Geometry,
Temperature, Density
4.5 6.5 8.5
10.5 12.5
Wavelength (mm)
Observations of warm H2 gas will constrain time
available to form gas giant planets.
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Factors Influencing Disk Evolution

• Stellar Properties
• Do high mass stars lose disks quicker?
• Does metallicity play a role in grain growth?
• Differences in specific angular momentum?
• Presence of companions
• Dynamical clearing of gaps?
• Stirring of planetesimals by giant planets?
• Formation environment
• cluster versus isolated star formation?

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The Sample of Solar-Type (FGK) Stars
Age N/Ntot Distance (pc)
Target
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Identifying Pre-Main Sequence Populations
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Activity Indicators for Main Sequence Stars
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How Does Our Sample Compare to GTOs?
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Formation and Evolution of Planetary Systems
The Legacy

• Library of SEDs for over 300 stars with ages
  3-3000 Myr
• SIRTF data plus ancillary optical, infrared, and
  sub-millimeter.
• Analysis tools for use by community
• model photospheres, grain properties, dynamical
  simulations.
• Basic Science Results
• timescales for formation evolution of planetary
  systems.
• Enhanced photometric calibration
• secondary standards, signal derivation, low-level
  errors.
• Unique software for pointed observations
• optimum coadding, photometric/spectral
  extraction.
• All manner of discoveries requiring follow-up by
  entire community!

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Summary of Planned SIRTF Observations
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Formation and Evolution of Planetary Systems
The Ancillary Database

• TYCHO/Hipparcos Database
• Proper motions and B-/V-band photometry.
• 2MASS Database
• JHK Complementary photometry.
• Optical Spectroscopy (Bok 90/MMT/Palomar/ESO)
• Spectral type, metallicity activity indices.
• Mid-infrared imaging (MMT/Palomar/Keck/NTT/VLT)
• Reality check high resolution follow-up.
• Sub-mm surveys (HHT SEST)
• Detect coldest dust follow-up interferometry.

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Structure and Composition of Debris Disks

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0.44-160 um Spectral Energy Distribution
POSS
2MASS
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CaII HK spectrum
25 um image
5-40 um spectrum
30
1300 um
2.2 um
60 um image
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Characterizing Planetary Systems Our Dust Disk
in Time
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Dust Opacity Effects of Size and Composition
shown at R100 (Henning et al. 2000)
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Effects of Giant Planets on Dust Distributions
Column density of 23 mm dust in particles/AU2
(taken from Liou Zook, 1999).
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The Formation Evolution of Planetary Systems
Placing Our Solar System in Context
Painting courtesy of William Hartman, Planetary
Science Institute, Tucson, AZ.

• We look forward to working with the community
  through the SIRTF Legacy Science Program and
  participating in the exciting discoveries sure to
  be made!
• http//gould.as.arizona.edu/feps