T Tauri and Debris Disks Rene Liseau Protostars

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

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

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

Disks in Time IRAS 1983 HST 1993 ISO 1995 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`´ Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

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

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

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

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 IRS 5 outflow source Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

T Tauri Disks - Sizes Fridlund et al. 2002 Size scale (AU) Tracer (mode) Reference 20000 5000 - 10000 1400 <500 45 + 1600 200 7000 5000 4000 - 6000 1200 4000 5000 2500 CS (1 - 0) (S) 13 CO (1 - 0) (S) C 18 O (1 - 0) (I) 1. 4 mm (I) mm, cm (I) 0. 8 mm (I) H 13 CO+ (1 - 0) (S) 0. 7 - 1 mm (S) C 18, 17 O (2 - 1) (S) 13 CO (1 - 0) (I) H 13 CO+ (1 - 0) (I) H 12, 13 CO+ (1 - 0) (S, I) C 18 O+ (1 - 0) (I) Kaifu et al. 1984 Fridlund et al. 1989 Sargent et al. 1988 Woody et al. 1989 Keene & Masson 1990 Lay et al. 1994 Mizuno et al. 1994 Ladd et al. 1995 Fuller et al. 1995 Ohashi et al. 1996 Saito et al. 1996 Hogerheijde et al. 1997, 98 Momose et al. 1998 Size depends on frequency/mode of observation Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

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

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

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

T Tauri Disks - Masses Lower limit: 0. 001 to 1 MSun (mm/submm continuum) How good are these numbers? Do we understand disks? Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

T Tauri Disks - Masses Assume optically thin emission at long wavelengths (mm+) monochromatic flux Fn ~ kn T spherical dust grains in equilibrium with stellar radiation achieve Qabs(n)/a = Q 0 nb T(a, R) = (h/k) p 1/(4+b) (L/a R 2)1/(4+b) p = (Qvis/Q 0) c 2/(32 p 2 h (3+b)! Sm m–(4+b) ) i. e. b = 0 => T ~ R-0. 50 b = 1 => T ~ R-0. 40 b = 2 => T ~ R-0. 33 Stockholm Observatory T ~ R-2/(4+b) kn ~ nb GENIE - workshop: Leiden, 3 -6 June 2002 page

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

T Tauri Disks - Masses Opacities k(n) Gas-to-dust 100? Stockholm Observatory Beckwith et al. 2000 GENIE - workshop: Leiden, 3 -6 June 2002 page

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

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

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

T Tauri Disks - Structure Steady Disks around Single Stars Boundary Conditions in : boundary layer, magnetosphere out: ? , interstellar turbulence? Viscosity MHD/rotation Opacity k = k(r, 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 (2 D) Stockholm Observatory Hawley & Balbus 1995 GENIE - workshop: Leiden, 3 -6 June 2002 page

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

T Tauri Disks - Chemistry Molecular abundances (rel. H 2) Species Lk. Ca 15 TW Hya CO HCO+ H 13 CO+ DCO+ CN H 13 CN HNC DCN CS H 2 CO CH 3 OH N 2 H+ H 2 D+ 3. 4(-7) 5. 6(-12) <2. 6(-12) …. 2. 4(-10) 3. 1(-11) …. …. …. 8. 5(-11) 4. 1(-11) <3. 7(-10) <2. 3(-11) <1. 5(-11) 5. 7(-8) 2. 2(-11) 3. 6(-13) 7. 8(-13) 1. 2(-10) 1. 6(-11) <8. 4(-13) <2. 6(-12) <7. 1(-14) …. <7. 1(-13) <1. 9(-11) <1. 8(-11) <7. 8(-12) Thi 2002 Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

T Tauri Disks - Evolution Time scales (viscous accretion disk) tdyn ~ a ttherm ~ a (H/R)2 tvisc tdyn ~ 1/WKepler Stockholm Observatory and a ~ 10 -3 - 10 -2 GENIE - workshop: Leiden, 3 -6 June 2002 page

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

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

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

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 MMoon (small dust) Pre-IRAS Solar system Zodi US Navy Chaplain G. Jones 1855 AJ 4, 94 Vega Blackwell et al. 1983 Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

THE Debris Disk – b Pictoris Sp. Type Distance Age Metallicity Disk size Disk Mass A 5 V Hipparcos Input Catalogue 1992 19. 3(0. 2) pc Hipparcos Catalogue 1997 15(5) Myr Song et al. 2001 solar Holweger & Rentzsch-Holm 1995 1835 AU NE 1450 AU SW Larwood & Kalas 2001 dust: >0. 44 MEarth Chini et al. 1991 gas: see below Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

b 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 line [C I] 370 mm [C I] 609 mm [C II] 157 mm [O I] 63 mm [Si II] 35 mm [Fe II] 26 mm rel. flux (line/Na D) 3 10 -7 2 10 -7 1 10 -2 dominates the cooling 2 10 -3 1 10 -3 6 10 -5 cf also Kamp & van Zadelhoff 2001, van Zadelhoff 2002 Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

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

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

THE Debris Disk – b 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. Ca. II HK and. . . Stockholm Observatory slit height 8´´ GENIE - workshop: Leiden, 3 -6 June 2002 page

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

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

THE Debris Disk – b Pictoris SCUBA JCMT 850 mm SIMBA SEST 1200 mm Holland et al. 1998 Peak position Peak flux Deconvolved size +0. 8, +9. 7 arcsec 58. 3(6. 5) m. Jy/beam 22´´ x 11´´ 0, 0 48. 8(1. 2) m. Jy/beam 26´´ x 10´´ Blob position Position angle Distance Flux -21, -26 arcsec 39. 6 deg 34´´ 19. 1(6. 5) m. Jy/beam -26, -44 arcsec 31. 5 deg 52´´ 19. 7(4. 2) m. Jy/beam Ratio 3. 0(1. 1) 2. 5(0. 5) Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

THE Debris Disk – b Pictoris Blob real? If so, associated with b Pic? Assume opacity exponents a for Blob and b for b Pic R 1200/R 850 = (850/1200)b-a b - a = 0. 53 (+0. 38, -0. 68) if b = 0. 8 (Wyatt & Dent 2002) a = 0. 3 then a ~ b? Stockholm Observatory a = [-0. 11, 0. 65] GENIE - workshop: Leiden, 3 -6 June 2002 page

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

Debris Disks and Planets Disks have non-homogeneous structure – not simple power law distributions because of planet(s)? a Lyr 1. 3 mm (Pd. B) Model: excentric ``Jupiter´´ Wilner et al. 2002 Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

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

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

Disks and GENIE Angular resolution of order 2. 5 (lmm)/b 100 m mas Debris disks generally at l > 25 mm Laureijs et al. 2002 L-band (1000 K), N-band (300 K) T Tauri disk: Debris disk: min(kscat, kabs) 0. 4 AU 3 mas 1. 2 AU 60 mas T Tauri disk: Debris disk: hot telescope/sky 9 AU 60 mas 25 AU 1. 2 arcsec L-band: N-band: Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

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

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

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

b 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 line [C I] 370 mm [C I] 609 mm [C II] 157 mm [O I] 63 mm [Si II] 35 mm [Fe II] 26 mm relative flux 3 10 -7 2 10 -7 1 10 -2 2 10 -3 1 10 -3 6 10 -5 cf also Kamp & van Zadelhoff 2001, van Zadelhoff 2002 Stockholm Observatory GENIE - workshop: Leiden, 3 -6 June 2002 page

b Pic: Atomic Gas Mass -2 Disk Absorption Line: N(Na) = 6 1010 cm @systemic/stellar velocity -6), then if. EW(Na. D 2) Na/H solar=(2 10 9. 4 mÅ* 17 g-2 16 M(Na) 2 10 N(HI) = 3 10 cm * [M(dust) 2 1027 g] **cf. et al. et 1995, cf. Freudling Vidal-Madjar al. 1986, AA 301, 231: N(HI) 1019325 cm-2 AA 167, Disk Emission Line: EW(Na. D 2) = 0. 72 mÅ (disk) = 8. 8 deg [r 0(Na. D) = 30 AU, H 0(disk) = 4. 6 AU]* *cf. Z(x) = 0. 055 rmax x 0. 75 , x = r/ rmax Stockholm Observatory rmax = 120 AU GENIE - workshop: Leiden, 3 -6 June 2002 page