Transcript Power-point version of presentation

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
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
rom Protostellar Disks to Mature Planetary Systems
Placing Our Solar System
in Context with SIRTF
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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:
»
»
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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
Evolution of inner accretion disks as traced by near-IR excess (Hillenbrand & Meyer, in
preparation).
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.
SIRTF Legacy Science: The Formation
and Evolution of Planetary Systems
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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.
Evolution of Dust Mass in Small Grains
Tracing the Evolution of the Gas:
Geometry, Temperature, &
Density
4.5
6.5
8.5
10.5
Wavelength (mm)
Observations of warm
H2 gas will constrain
time available to form
gas giant planets.
12.5
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?
The Sample of Solar-Type (FGK) Stars:
Age
3-10 Myr
N*/Ntot
50/
~140
10-30 Myr 50/
~110
30-100
50/
Myr
~130
100-300
50/
Myr
~100
0.3-1 Gyr 50/
~1000
1-3 Gyr
50/
~1000
Distance (pc)
80-160
Target
20-60
Tau, Oph, Cha,
Lup, Upper Sco
Tau, Oph, Cha,
Lup, Cen Crux
IC 2602 &
Alpha Per
Ursa Major,
Castor, Pleiades
Field stars, Hyades
20-60
Field stars
60-160
40-180
20-120
Identifying Pre-Main Sequence Populations:
Activity Indicators for Main Sequence Stars:
How Does Our Sample Compare to GTOs?
Formation and Evolution of Planetary
Systems: The Legacy
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Library of SEDs for over 300 stars with ages ~ 3-3000 Myr:
» SIRTF data plus ancillary optical, infrared, and sub-millimeter.
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Analysis tools for use by community:
» model photospheres, grain properties, dynamical simulations.
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Basic Science Results:
» timescales for formation & evolution of planetary systems.
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Enhanced photometric calibration:
» secondary standards, signal derivation, low-level errors.
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Unique software for pointed observations:
» optimum coadding, photometric/spectral extraction.
All manner of discoveries requiring follow-up by entire community!
Summary of Planned SIRTF
Observations
Instr.
N*
SNR (F[star]) Objectives
IRAC
300
MIPS
300
>>50 from
3.6-8.0 mm
>50 at 24 mm
>5 at 70 mm
>50 5-14mm
>10 14-40 mm
>3 for 2x10-4
M< H2 gas
IRS-Lo 300
IRS-Hi 50
Measure phot. &
search for hot dust.
Complete census
of cool dust.
Inflections in SED
& dust properties.
Disk gas mass and
dust features.
Formation and Evolution of Planetary
Systems: The Ancillary Database
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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.
Structure and Composition of Debris
Disks
0.44-160 um Spectral Energy Distribution
POSS
2MASS
5’
CaII H&K spectrum
25 um image
5-40 um spectrum
30’
2.2 um
60 um image
30’
1300 um
Characterizing Planetary Systems: Our Dust Disk in Time
Dust Opacity: Effects
of Size and
Composition shown at
R=100 (Henning et al.
2000)
Effects of Giant Planets on Dust Distributions
Column density of 23 mm dust in particles/AU2 (taken from Liou & Zook,
1999).
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