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

2. 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.

3. From Protostellar Disks to Mature Planetary Systems

4. Placing Our Solar System in Context with SIRTF  First Mission of NASA’s “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.edu

5. Evolution of inner accretion disks as traced by near-IR excess (Hillenbrand & Meyer, in preparation).

6. 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.

7. 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.

8. Evolution of Dust Mass in Small Grains

9. Tracing the Evolution of the Gas: Geometry, Temperature, & Density Observations of warm H 2 gas will constrain time available to form gas giant planets. 4.5 6.5 8.5 10.5 12.5 Wavelength (  m)

10. 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?

11. The Sample of Solar-Type (FGK) Stars: Age N * /N tot Distance (pc) Target

12. Identifying Pre-Main Sequence Populations:

13. Activity Indicators for Main Sequence Stars:

14. How Does Our Sample Compare to GTOs?

15. 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!

16. Summary of Planned SIRTF Observations

17. 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.

18. Structure and Composition of Debris Disks

19. 2.2 um 25 um image 1300 um 5-40 um spectrum CaII H&K spectrum 0.44-160 um Spectral Energy DistributionPOSS2MASS 5’ 30’ 60 um image 30’

20. Characterizing Planetary Systems: Our Dust Disk in Time

21. Dust Opacity: Effects of Size and Composition shown at R=100 (Henning et al. 2000)

22. Column density of 23  m dust in particles/AU 2 (taken from Liou & Zook, 1999). Effects of Giant Planets on Dust Distributions

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