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Evolution of Dust Disks in Planetary Systems

Explore the lifetime of dust disks around stars, from planet building to debris disks. Learn the differences between primordial and debris disks, with insights on star and planet formation. Study constraints on planet-formation timescales and disk lifetimes at different radii.

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Evolution of Dust Disks in Planetary Systems

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  1. The Lifetime ofDust DisksLynne Hillenbrand. . . . . . . . . . . Caltech

  2. 10 105 yr Disk/wind Lstar 104 yr Planet building 107 yr 109 yr 1 Planetary system 100 AU Main sequence Cloud collapse 8,000 5,000 2,000 Tstar (K) Star and planet formation/evolution [Beckwith & Sargent 1996]

  3. [04302+2247] Before/during/afterprotostellar collapse [B68] [Padgett et al.] [ONC “proplyd”] [Alves, Lada, Lada] [McCaughrean et al.; Stauffer et al.]

  4. Not so much later: Debris disks

  5. What is the difference between “primordial” and “debris” disks? Debris Primordial [Dullemond and Pontoppidian]

  6. POST ACCRETION ice giant formation DEBRIS DIKS Spitzer legacy science:The formation and evolution of planetary systems 3 Myr – 3 Gyr • Birth of planetary embryos: Characterize transition from primordial to debris dust disks. • Growth of gas giant planets: Constrain time scale for gas disk dissipation. • Mature solar system evolution: Examine diversity of planetary systems based on debris disks.

  7. Evolution of our own dust disk in time [D. Backman] Model spectral energy distribution Is our solar system common or u n i q u e ?

  8. NIR MID FIR sub-m Circumstellar disk and SED In anobserved SED, each wavelength traces a distinct temperature, and different temperatures correspond to different radii in disk (cooler at larger radii). 0.1 1.0 10.0 – 40.0 100 AU Temperature 1 10 100

  9. NIR – MID Young (< 30 Myr) disks 0.1 – <1.0 AU A Spitzer instrument to detect these disks: IRAC(3.6 m, 4.5 m, 8.0 m)

  10. MIR FIR Warm disks 10.0 – 40.0 A Spitzer instrument to detect these disks:IRS(10 – 35 m)

  11. FIR Cold outer disks ~20 – 100 AU A Spitzer Instrument to detect these disks:MIPS(24 – 160 m)

  12. Constraints on planet-formation time scalesInner disk dissipationData suggest <3–10 Myr as maximum accretion disk lifetime. Typical lifetime for material at <0.1 AU is <3 Myr.Mid-disk dissipationMaximum disk lifetime for terrestrial planet material at 1 AU is also <10 Myr. Compare with meteoritic evidence suggesting Earth formed in <10 Myr with moon-forming impact occurring at 30 Myr.Outer disk dissipation and re-generationPrimordial disk lifetimes as yet unconstrained. Debris disk lifetimes consistent with expectations from self-sustaining collisional cascade.

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