Debris disks Basic properties Observational methods & constraints

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Presentation transcript:

Debris disks Basic properties Observational methods & constraints Why “debris”? Structures Alexis Brandeker, Lecture 6 in star formation mini-course Resonance Line Scattering in the beta Pic Disk

Discovery of debris disks From Backman & Parece 1993, PPIII, 1253 Resonance Line Scattering in the beta Pic Disk

Discovery of debris disks From Backman & Parece 1993, PPIII, 1253 Resonance Line Scattering in the beta Pic Disk

First disk spatially resolved: b Pictoris Discovery image by Smith & Terrile 1984 (Sci. 226, 1421) 500 AU Resonance Line Scattering in the beta Pic Disk

Properties Large (up to 1000 AU) dusty disks found around young main-sequence stars ~ 10 Myr – 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 Resonance Line Scattering in the beta Pic Disk

”The fabulous four” at 850m 3.2 pc 7.7 pc 7.7 pc 20 pc Resonance Line Scattering in the beta Pic Disk

Resonance Line Scattering in the beta Pic Disk

b Pictoris in scattered light Resonance Line Scattering in the beta Pic Disk

Resonance Line Scattering in the beta Pic Disk

Resonance Line Scattering in the beta Pic Disk

Resonance Line Scattering in the beta Pic Disk

Resonance Line Scattering in the beta Pic Disk

Resonance Line Scattering in the beta Pic Disk

Resonance Line Scattering in the beta Pic Disk

ZAMS 20 Myr 30 Myr Barrado y Navascués 1999 50 Myr

Resonance Line Scattering in the beta Pic Disk

Why “debris”? From Artymowicz 1997, AR 25:175 Resonance Line Scattering in the beta Pic Disk

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

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

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

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

Dust disk lifetimes From Haisch, Lada & Lada 2001, ApJ, 553, 153 Resonance Line Scattering in the beta Pic Disk

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

mm/submm observations Liseau & Artymowicz 1998, A&A 335, 935 Resonance Line Scattering in the beta Pic Disk

Edge-on  absorption!

Gas in emission Sodium D1/2 lines toward b Pictoris Olofsson, Liseau & Brandeker 2001, ApJL 563 Sodium D1/2 lines toward b Pictoris Resonance Line Scattering in the beta Pic Disk

Dynamical studies... Stellar structure: M*=(1.75±0.1)Mo Gas dynamics: Mdyn=(1.40±0.05)Mo Discrepancy probably due to radiation pressure! Resonance Line Scattering in the beta Pic Disk

HR 4796A

b Pictoris in scattered light NE SW Resonance Line Scattering in the beta Pic Disk

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

1.2 mm (SEST/SIMBA) Liseau et al. 2003 Resonance Line Scattering in the beta Pic Disk

Asymmetris in gas disk VLT / UVES (Brandeker et al. 2004) We found lots of atomic and ionic metallic gas emission in the disk, extending to at least 320 AU radially from the star. VLT / UVES (Brandeker et al. 2004) Resonance Line Scattering in the beta Pic Disk

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

StarStrider [AU] Resonance Line Scattering in the beta Pic Disk