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Debris disks

Debris disks. Basic properties Observational methods & constraints Why “debris”? Structures. Alexis Brandeker, Lecture 6 in star formation mini-course. Discovery of debris disks. From Backman & Parece 1993, PPIII, 1253. Discovery of debris disks. From Backman & Parece 1993, PPIII, 1253.

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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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