Protoplanetary Disk * ELT *

Transcription

1 Protoplanetary Disk * ELT * Miwa Goto Max Planck Institute for Extraterrestrial Physics Garching, Germany

2 Observing CO vibrational band in Protoplanetary Disk angular resolution + IR high angular resolution 2 warm targets that is barely resolved so far spectral resolution + IR gas, not ice or dust molecules vibrational transitions kinematics high spectral resolution rotationally quiet molecules even better Here nearinfrared midinfrared H2, H3 +, CH4, C2H2 symmetric molecules without permanent dipole moment

3 What is CO vibrational band? Why CO is so special? # Element Solar photospheric abundance H He [0.93] 3 Li.05 Why sub-mm astronomers like it so much? yes, abundance is high but, why not OH or H2O? 4 Be.38 5 B C N O F Ne [7.93] Asplund 2009, ARAA

4 Let us start with rotational transition reduced mass makes this into this +!!2 =!

5 + =!!! 2!! 2! 2!!! 2!! smaller one H O H F all looks more like H H C H Cl H

6 Rotational Energy levels r mrv = J rotational angular momentum (again ) I = μr 2 moment of inertia E = mv 2 2 m J = ( ) 2 2 mr J 2 = 2mr 2 h 2 ΔE = ( J+) I the larger μ, the larger I energy gap is small easily excited even at low T easy to observe h 2 = J2 2I E = J ( J+) 2I correct answer not too bad

7 Hydride total mass reduced mass Δ J = from lowest ΔE OH cm 9 K HF cm 59 K HCl cm 30 K HBr cm 23 K non-hydride total mass reduced mass Δ J = form lowest ΔE CO cm 5.5 K CS cm 2.3 K (rule of thumb) the bigger, the easier to excite

8 ELT/METIS wrap up aperture 39 m 3 μm 5 μm 8 μm 4 μm HD, NH CO SO C λ/d 6 mas 26 mas 42 mas 74 mas at 50 pc 2.4 AU 4.0 AU 6.3 AU AU imaging 3-9 μm low-resolution spectroscopy R=, μm med-resolution spectroscopy R=0, μm high-resolution spectroscopy R=00, μm IFU

9 electron orbital m energy angular momentum Eelec = mv 2 = kr mrv = 4 δr Evib = μvb 2 = k(δr) μ(δr)vb = 5 vibrational k μ Erot = μvr μrvr = 6 rotational all scale μ 2 v δr μ = R m Vb Vr δr m = Vb R μ mm v μ = m Vr Vr R = Vb δr proton / electron mass ratio ~R Oka, Takeshi Vr m = ( ) /4 μ Vb Erot m = ~ Evib μ 0 μm 00

10 R-branch ΔJ = P-branch ΔJ = - v = 2 overtone 2.3 μm Δv = 2 fundamental Δv = 4.6 μm mm J = 2 0 v = v = 0 infrared spectroscopy covers many lines in one shot

11 Population diagram v = 2 NJ Boltzmann distribution = exp(- ) gj N0 Qt ΔEJ kt partition function ΔEJ Qt = gj Σ exp(- ) J kt angular momentum statistical weight just normalization factor so that N0 = Σ NJ J ΔEJ { 4 3 cold warm gj = 2J+ 9 7 NJ ln = ln - gj N0 Qt T ΔEJ k y = b - a x 2 J = 0 v = 0 5 3

12 Population diagram NJ ln = ln - gj N0 Qt T ΔEJ k total column N0 [cm-2] excitation temperature [K] LTE+ optically thin or not y = b - a x N0 ln Qt - T

13 Mindmap of CO protoplanetary disks Observation R = 680 R = Carr 89 Najita 96 WL 6 - Shoulder - CO v=2-0 + Keck / NIRSPEC Subaru / IRCS Gemini S / Phoenix VLT /CRIRES m class 8-m class - Precision Modeling Najita 03 - CO v=-0 Carr 07 - corotational radius - Hot Jupiter Herbig Ae/Be M* < 2Mo Younger analog + UV + photoevaporation + disk atmosphere T Tauri stars M* < 2Mo Solar analog Transition Disks - Salyk 09 CRIRES LP HR8799 Vega beta Pic Chemistry Imaging Something wrong... - Pontoppidan 08 - astrometry - Herczeg - Bast - Blake & Boogert 04 - Brittain 03, 07 - van der Plas 09, 5 - Goto 06, Brown 3 Banzatti 5 No double peaks Slow disk wind Envelope disk Class I/II no difference Theory - Scoville 80 collisional excitation - Krotkov 80 UV excitation Tvib ~ Trad - Clarke 0 UV switching - Calvet 0 Temperature flip - Glassgold, Najita 09 - Gorti, Hollenbach 08 x-ray photoionization Outburst - Rettig 05 - Goto + McNeil s Nebula EX Lup Thi, Kamp, Woitke ProDiMo Disk chemistry

14 Techniques 2 spectroscopy imaging λ x 3 monitoring t

15 2 imaging x Target spatial scales photoevaporation gravitational radius rg ~ GM* cs 2 7 x 0-8 cm 3 g - s cm/s 2 x 0 30 g ~.3 x 0 4 cm ~ 9 AU 2 spiral arms / planet formation 0. gravitational instability rq = R M d M* ~0 AU if disk is 00 AU so both 0. at 00 pc away ELT is not just bigger and better The telescope overcomes the barriers for the first time

16 2 imaging x HD 4569 A Herbig Ae/Be Adaptive Optics, Subaru, R=20000 high resolution spectroscopy virtual coronagraphy Goto et al. 2006

17 HD Herbig Ae/Be Adaptive Optics VLT / CRIRES, R=00,000 stellar continuum

18 HD Herbig Ae/Be Adaptive Optics VLT / CRIRES, R=00,000 stellar continuum subtracted

19 HD 4569A HD near side brighter IFU changes life much easer

20 ALMA vs CRIRES HD Herbig Ae star ALMA / 375m / 870μm 6000 m CRIRES / 8m / 4.6μm 39 m Pineda et al. 204 so far CRIRES wins like factor of 3-0 we still have to see

21 2 imaging x + spectroscopy λ Goto et al. 202 Teq < 90 K Trot > 500 K UV fluorescence imaging confirmation of hot disk atmosphere

22 3 monitoring t + spectroscopy λ EX Lup, 2008 outburst 7 days 3 days AU Hot spot spiral into the star Goto et al. 20

23 3 Monitoring T Tauri star (M ) 7 yr /4 turn 0 AU Herbig Ae/Be star (2M ) 2 yr 5 yr /4 turn 5 AU 0 AU

24 with ELT / METIS spectroscopy λ + 2 imaging x + 3 monitoring t Gap in the disk

25 spectroscopy λ + 2 imaging x + 3 monitoring t Bridge in the disk

26 3 Monitoring Im Lup, Oeberg 5 ALMA delivered an image ELT will make it move

27 thank you for your attention