1. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 1 T Tauri and Debris Disks Rene´ Liseau Pawel Artymowicz Alexis Brandeker Malcolm Fridlund Göran Olofsson Protostars & Planets IV, Mannings, Boss & Russell eds. B. Zuckerman, ARAA 2001, 39: 549 W-F Thi 2002, PhD thesis, Leiden G-J van Zadelhoff 2002, PhD thesis, Leiden

2. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 2 Disks in Time P.S. Laplace 1796, 1799 Exposition du systeme du monde Mechanique celeste I. Kant 1755 Allgemeine Naturgeschichte und Theorie des Himmels

3. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 3 Disks in Time JE Keeler 1895 ApJ 1: 416

4. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 4 Disks in Time T Tauri Disks: around young stars (0.1 - 10 Myr) of half a solar mass (0.1 - 1 Msun) at 150 pc distance (50 - 450 pc) in and/or near molecular clouds ``accretion disks´´ Debris Disks: around young MS-stars (10 - 400 Myr) of about a solar mass (1 - 2 Msun) at 20 pc distance (3 - 70 pc) in the general field ``Vega-excess stellar disks`´ IRAS 1983ISO 1995HST 1993

5. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 5 Frequency of Disks High Rate of occurence around young stars NGC 2024 86% Trapezium cluster 80% IC 348 65% Haisch et al. 2001 BDs in Trapezium cluster 65% Muench et al. 2001

6. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 6 Disk Images

7. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 7 HH 30 in L 1551 (Taurus) T Tauri Disk with Jet

8. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 8 T Tauri Disks - Sizes R=7000 AU Fridlund et al. 2002 (mm line data - single dish) White et al. 2000 (mid- & far IR line + cont. - ISO) L 1551 IRS5 outflow source

9. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 9 T Tauri Disks - Sizes Size scale (AU)Tracer (mode)Reference 20000CS (1- 0) (S)Kaifu et al. 1984 5000 - 10000 13 CO (1- 0) (S)Fridlund et al. 1989 1400C 18 O (1- 0) (I)Sargent et al. 1988 <5001.4 mm (I)Woody et al. 1989 45 + 1600mm, cm (I)Keene & Masson 1990 2000.8 mm (I)Lay et al. 1994 7000H 13 CO + (1- 0) (S)Mizuno et al. 1994 50000.7 - 1 mm (S)Ladd et al. 1995 4000 - 6000C 18, 17 O (2- 1) (S)Fuller et al. 1995 1200 13 CO (1- 0) (I)Ohashi et al. 1996 4000 H 13 CO + (1- 0) (I)Saito et al. 1996 5000 H 12, 13 CO + (1- 0) (S, I)Hogerheijde et al.1997, 98 2500 C 18 O + (1- 0) (I)Momose et al. 1998 Fridlund et al. 2002 Size depends on frequency/mode of observation

10. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 10 T Tauri Disks - Sizes Two Disks: separation = 40 AU & R = 5 AU Rodriguez et al. 1998 (7 mm cont. - VLA Interferometer ) L 1551 IRS5 outflow source

11. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 11 T Tauri Disks - Sizes Summarising: T Tauri/HABE disks 50 - 100 AUDust: mm-continuum interferometry 100 - 300 AUDust: scattered stellar light 300 AUGas: CO lines (evidence for Kepler rotation) Silhouettte disks (``proplyds´´) up to 1000 AUDust: scattered stellar light

12. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 12 T Tauri Disks - Sizes & Masses

13. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 13 T Tauri Disks - Masses Lower limit: 0.001 to 1 M Sun (mm/submm continuum) How good are these numbers? Do we understand disks?

14. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 14 T Tauri Disks - Masses Assume optically thin emission at long wavelengths (mm+) monochromatic flux F ~  T spherical dust grains in equilibrium with stellar radiation achieve T(a, R) = (h/k) p 1/(4+  ) (L/a R 2 ) 1/(4+  ) Q abs ( )/a = Q 0  p = (Q vis /Q 0 ) c 2 /( 32  2 h (3+  )!  m m –(4+  ) ) i.e. T ~ R -2/(4+  )  = 0 => T ~ R -0.50  = 1 => T ~ R -0.40  = 2 => T ~ R -0.33  ~ 

15. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 15 T Tauri Disks - Masses parameters  0 and  require knowledge of grain chemical composition shape size size distribution... but  a good diagnostic? Larsson et al. 2000, 2002 White et al. 2000

16. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 16 T Tauri Disks - Masses Beckwith et al. 2000 Opacities  Gas-to-dust 100?

17. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 17 T Tauri Disks - Structure Lynden-Bell & Pringle 1974

18. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 18 T Tauri Disks - Structure D´Alessio et al. 1999 40 SEDs

19. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 19 T Tauri Disks - Structure Steady Disks around Single Stars ESO-AO Brandeker et al. 2001 VW Cha: tidally truncated disk: 60 AU

20. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 20 T Tauri Disks - Structure Steady Disks around Single Stars Boundary Conditions in : boundary layer, magnetosphere out: ?, interstellar turbulence? Viscosity MHD/rotation Hawley & Balbus 1995 Opacity , T,...) Models: Adams & Shu 1986 (flat) Kenyon & Hartmann 1987 (flared) Malbet & Bertout 1991 (vertical structure) D´Allessio et al. 1998,... 2001 Aikawa & Herbst 1998 (chemistry) Nomura 2002 (2D)

21. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 21 T Tauri Disks - Make up T Tauri disks consist of gas and dust what components? in what proportions? van Zadelhoff 2002 13 CO (1) HCO + (5) HCN (5) CO (200) HCO + (200) HCN (200 ) LkCa 15TW Hya

22. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 22 T Tauri Disks - Chemistry Molecular abundances (rel. H 2 ) Species LkCa 15TW Hya CO3.4(-7)5.7(-8) HCO + 5.6(-12)2.2(-11) H 13 CO + <2.6(-12)3.6(-13) DCO + ….7.8(-13) CN2.4(-10)1.2(-10) HCN3.1(-11)1.6(-11) H 13 CN….<8.4(-13) HNC….<2.6(-12) DCN….<7.1(-14) CS8.5(-11)…. H 2 CO4.1(-11)<7.1(-13) CH 3 OH<3.7(-10)<1.9(-11) N 2 H + <2.3(-11)<1.8(-11) H 2 D + <1.5(-11)<7.8(-12) Thi 2002

23. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 23 T Tauri Disks - Evolution Time scales (viscous accretion disk) t dyn ~  t therm ~  (H/R )2 t visc t dyn ~ 1/  Kepler and  ~ 10 -3 - 10 -2

24. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 24 T Tauri Disks - Evolution Disk dispersal and disk lifetimes Hollenbach et al. 2000 Mass accretion evolution Calvet et al. 2000

25. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 25 T Tauri Disks to Debris Disks Spangler et al. 2001 f d =  L IR /L vs stellar age

26. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 26 Debris Disks - Images P. Kalas

27. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 27 Debris Disks - Properties debris (collision products) or particulate (gas free) percentage of Main Sequence stars (?) (observationally) biased towards Spectral Type A for (detectable) ages <400 Myr Habing et al. 1999, 2001 disk sizes 100 to 1000 AU disk masses >1 to 100 M Moon (small dust) Pre-IRAS Solar system Zodi US Navy Chaplain G. Jones 1855 AJ 4, 94 Vega Blackwell et al. 1983

28. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 28 THE Debris Disk –  Pictoris Sp. TypeA5 V Hipparcos Input Catalogue 1992 Distance19.3(0.2)  pc  Hipparcos Catalogue 1997 Age15(5) Myr Song et al. 2001 Metallicitysolar Holweger & Rentzsch-Holm 1995 Disk size1835 AU NE 1450 AU SW Larwood & Kalas 2001 Disk Mass dust: >0.44 M Earth Chini et al. 1991 gas: see below

29. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 29  Pic Disk Model: Gas Best fit model (self consistent photoionisation calculation) to EMMI data with observed emission line flux Na D 2 1.5 10 -13 erg s -1 cm -2 linerel. flux (line/Na D) [C I]370  m3 10 -7 [C I]609  m2 10 -7 [C II]157  m1 10 -2 dominates the cooling [O I] 63  m2 10 -3 [Si II] 35  m1 10 -3 [Fe II] 26  m6 10 -5 cf also Kamp & van Zadelhoff 2001, van Zadelhoff 2002

30. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 30  Pictoris New: gas disk extension to >300 AU in e.g. Na I D 2 Olofsson et al. 2001 model model obser- vation VLT 2002 =>

31. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 31

32. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 32 THE Debris Disk –  Pictoris Presence of substantial amounts of H 2 debated Thi 2002 Presence of atomic gas – no doubt Olofsson et al. 2001 new VLT data reveal disk flaring in e.g. CaII HK and... slit height 8´´

33. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 33 THE Debris Disk –  Pictoris The VLT Disk Spectrum (340 – 390 nm) only permitted lines no Fe II, no H I Fe Imultiplets 4, 5, 40, 41 Ca IIH & K TbcNi I, Ti I, V II, Cr I, Co I, Mn I, Ru I, Ce II, Tm I

34. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 34 THE Debris Disk –  Pictoris 1200  m (SEST) 850  m (JCMT)...and the ``Blob´´

35. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 35 THE Debris Disk –  Pictoris SCUBA JCMT 850  mSIMBA SEST 1200  m Holland et al. 1998 Peakposition+0.8, +9.7 arcsec 0, 0 Peak flux58.3(6.5) mJy/beam 48.8(1.2) mJy/beam Deconvolved size22´´ x 11´´26´´ x 10´´ Blob position-21, -26 arcsec -26, -44 arcsec Position angle39.6 deg 31.5 deg Distance34´´52´´ Flux19.1(6.5) mJy/beam 19.7(4.2) mJy/beam Ratio3.0(1.1)2.5(0.5)

36. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 36 THE Debris Disk –  Pictoris Blob real? If so, associated with  Pic? Assume opacity exponents  for Blob and  for  Pic R 1200 /R 850 = (850/1200)   = 0.53 (+0.38, -0.68) if  = 0.8 (Wyatt & Dent 2002) then  = 0.3  ?  = [-0.11, 0.65]

37. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 37 Debris Disks and Planets Disks have non-homogeneous structure – not simple power law distributions because of planet(s)?  Pic Keck 18  m Wahhej et al. 2002 Heap et al. 2000

38. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 38 Debris Disks and Planets Disks have non-homogeneous structure – not simple power law distributions because of planet(s)? Wilner et al. 2002  Lyr 1.3 mm (PdB) Model: excentric ``Jupiter´´

39. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 39 Debris Disks and Planets Do ``Planet-Stars´´ have disks? 55 Cnc No! Jayawardhana et al. 2002  CrBtbc Trilling et al. 2000 HD 210277tbc  Eri a border case? Hatzes et al. 2000

40. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 40 Disks: Open Questions Grain growth: from micron to cm size from cm to 100 m+ size Time of (giant) planet formation termination of planet migration Processes/time scales of disk dispersal formation and evolution of debris disks Role of stellar multiplicity free-floating planets

41. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 41 Disks and GENIE Angular resolution of order 2.5 (  m )/b 100m mas Debris disks generally at > 25  m Laureijs et al. 2002 L-band (1000 K), N-band (300 K) L-band: min (  scat,  abs ) T Tauri disk: 0.4 AU 3 mas Debris disk:1.2 AU60 mas N-band:hot telescope/sky T Tauri disk: 9 AU60 mas Debris disk:25 AU1.2 arcsec

42. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 42

43. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 43

44. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 44 Debris Disks and Planets Vega  Eri

45. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 45  Pic Disk Models Best fit model (self consistent photoionisation calculation) to EMMI data with observed emission line flux Na D 2 1.5 10 -13 erg s -1 cm -2 linerelative flux [C I]370  m3 10 -7 [C I]609  m2 10 -7 [C II]157  m1 10 -2 [O I] 63  m2 10 -3 [Si II] 35  m1 10 -3 [Fe II] 26  m6 10 -5 cf also Kamp & van Zadelhoff 2001, van Zadelhoff 2002

46. Stockholm Observatory GENIE - workshop: Leiden, 3-6 June 2002 page 46  Pic: Atomic Gas Mass Disk Absorption Line: @systemic/stellar velocity EW(NaD2) = 9.4 mÅ*  M(Na)  2  10 17 g [M(dust)  2  10 27 g] * cf. Vidal-Madjar et al. 1986, AA 167, 325 Disk Emission Line: EW(NaD2) = 0.72 mÅ  (disk) = 8.8 deg [r 0 (NaD) = 30 AU, H 0 (disk) = 4.6 AU]* *cf. Z(x) = 0.055 r max x 0.75, x = r/ r max r max = 120 AU N(Na) = 6  10 10 cm -2 if Na/H solar (2  10 -6 ), then N(HI) = 3  10 16 cm -2 * * cf. Freudling et al. 1995, AA 301, 231: N(HI)  10 19 cm -2