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Debris disks

Discover the structures and properties of debris disks found around young stars, essentially free of gas and dominating dust emissions. Learn about the observational methods and constraints in studying these dusty disks and why they are named "debris." Explore the discovery of the first spatially resolved disk around b.Pictoris and the evolution of debris disks from young to old stages. Gain insights into the gas dynamics, disk lifetimes, and asymmetries in gas disks. Delve into the stellar structures and dynamical studies to understand the discrepancies in mass calculations.

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Debris disks

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  1. Debris disks • Basic properties • Observational methods & constraints • Why “debris”? • Structures Alexis Brandeker, Lecture 6 in star formation mini-course

  2. Discovery of debris disks From Backman & Parece 1993, PPIII, 1253

  3. Discovery of debris disks From Backman & Parece 1993, PPIII, 1253

  4. First disk spatially resolved:b Pictoris Discovery image by Smith & Terrile 1984 (Sci. 226, 1421) 500 AU

  5. Properties • Large (up to 1000 AU) dusty disks found around young main-sequence stars ~ 10Myr – 1 Gyr • Dust disk mass M ~ 10-3 to a few MEarth. • Essentially free of gas • Cold; typically 30 – 300 K • Dominating dust emission from m to mm sized grains

  6. ”The fabulous four” at 850m 3.2 pc 7.7 pc 7.7 pc 20 pc

  7. b Pictoris in scatteredlight

  8. ZAMS 20 Myr 30 Myr Barrado y Navascués 1999 50 Myr

  9. Why “debris”? From Artymowicz 1997, AR 25:175

  10. Breakup of Parent Body   Frad/Fgrav  = 1 0.51 2.2 0.1 0.3 0.4

  11. Top view Orbit of Pluto-mass parent body before breakup Side view  = Elapsed time: 21 years Florida Dynamics Group

  12. Top view Side view  = Elapsed time: 569 years Florida Dynamics Group

  13. Subaru/COMICS (Y.Okamoto et al. 2004) Total (magenta) 0.1mm amorphous olivine (green) 2mm amorphous olivine (red) Crystalline forsterite (blue) Power-law continuum (cyan)

  14. Dust disk lifetimes From Haisch, Lada & Lada 2001, ApJ, 553, 153

  15. What about gas? Energy diagram of H 2 [Pollack et al. 1993] Total mass 30.0 Energy [K] 20.0 Core mass 10.0 Gas mass

  16. mm/submm observations Liseau & Artymowicz 1998, A&A 335, 935

  17. Edge-on  absorption!

  18. Olofsson, Liseau & Brandeker 2001, ApJL 563 Gas in emission Sodium D1/2 lines toward b Pictoris

  19. Dynamical studies... Stellar structure: M*=(1.75±0.1)Mo Gas dynamics: Mdyn=(1.40±0.05)Mo Discrepancy probably due to radiation pressure!

  20. HR 4796A

  21. b Pictoris in scatteredlight NE SW

  22. NE SW 24.3 m FWHM 5 arcsec 18.3 m 100 AU 11.7 m Gemini south / T-ReCS Telesco et al. 2005 pixel

  23. 1.2 mm(SEST/SIMBA) Liseau et al. 2003

  24. Asymmetris in gas disk VLT / UVES (Brandeker et al. 2004)

  25. Optical/IR disks Sub-mm rings/arcs Evolution: young vs. old debris Credit: M. Liu

  26. StarStrider [AU]

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