Michael R. Meyer Steward Observatory, The University of Arizona
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Steward Observatory, The University of Arizona
D. Backman (NASA-Ames, D.P.I.) , S.V.W. Beckwith (STScI), J. Bouwman (MPIA), T. Brooke (Caltech), J.M. Carpenter (Caltech), M. Cohen (UC-Berkeley), U. Gorti (NASA-Ames), T. Henning (MPIA), L. Hillenbrand (Caltech, D.P.I.), D. Hines (SSI), D. Hollenbach (NASA-Ames), J. Lunine (LPL), J.S. Kim (Steward), R. Malhotra (LPL), E. Mamajek (CfA), A. Moro-Martin (Princeton ), P. Morris (SSC), J. Najita (NOAO), D. Padgett (SSC), I. Pascucci (Steward), J. Rodmann (MPIA), W. Schlingman (Steward), M. Silverstone (Steward), D. Soderblom (STScI), J.R. Stauffer (SSC), B. Stobie (Steward), S. Strom (NOAO), D. Watson (Rochester), S. Weidenschilling (PSI), S. Wolf (MPIA), and E. Young (Steward).Placing Our Solar System in Context with the Spitzer Space Telescope
Silverstone et al.
See also Mamajek et al. 2004; Weinberger et al. 2004; Metchev et al. 2004.
3-10 Myr old IRAC.
10-30 Myr old IRAC.
Silverstone et al.
(ApJ, in press)
Cf. Wolk and Walter, 1996; Kenyon and Hartmann, 1995; Prato and Simon, 1995; Skrutskie et al. 1990.
Out of a sample of
> 70 stars 3-30 Myr old, 5 optically-thick disks, and no optically-thin disks.
* Some wTTs do have disks
not previously detected,
BUT only the younger ones
( ages < 3 to 6 Myr)
[ages are ~ uncertain]
* 1/2 the young ones lack disks, even at age 0.8 to 1.5 Myr
* Age is NOT the only variable
Big RED circle: has disk
Padgett et al., in prep; Cieza et al., in prep.
* Some wTTs have inner holes, but small fraction of systems.
* May be cleared by planet formation
* Infer that disk clearing is fast
* Planet formation is “fast or not at all”
Cieza et al., in prep.
Warm debris (perhaps 4-6 AU) around 30 Myr old sun-like star! Hines et al. (ApJ, in press); Mamajek et al. poster, this meeting.
Bouwman et al. (in preparation); cf. Beichman et al. (2005);
Song et al. (2005), Chen et al. (2005); Kenyon & Bromley (2004)
Solar-type stars in the Pleiades (age ~ 100 Myr) cessation of accretion (cf. C2D)
5 cases of excess at 24 & 33 mm; 2-3 probably real (not bkg)
Stauffer et al. 2005; Stauffer et al. poster, this meeting
GAS cessation of accretion (cf. C2D)
Cool Gas in Disks
Gorti & Hollenbach (2004); also Najita et al. poster, this mtg
GAS DETECTABLE HERE
=> No gas rich disk
(> 0.1 Mjup) detected.
=> 20 stars with ages 3-100 Myr
Hollenbach et al. (ApJ, 2005); Najita et al. poster, this mtg
MMSN = minimum mass solar nebula cessation of accretion (cf. C2D)
30+- 10 Myr
45 to ??? AU
Kim et al. 2005,
Hillenbrand et al. poster, this mtg;
cf. Bryden et al. 2005
700+- 300 Myr
20 to <100 AU
Kim et al. 2005; Hillenbrand et al. poster, this mtg
NB: less common at ages > 300 Myr than 70 mm (~ 50 K) detections
See also Bryden et al. (2005)
Backman et al. in prep; cf. Gomes et al. (2005); Strom et al. (2005),
Levison et al. (PPV), Kenyon & Bromley (2004).
FEPS excesses = extrasolar Late Heavy BombardmentsPreliminary Results: Debris Disk Lifetimes
< 0.1 0.3-1.0 1-10 30-100