calculating the infrared spectra of hot astrophysical molecules selac, may 2005 jonathan tennyson...
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Calculating the infrared spectra of hot astrophysical molecules
SELAC, May 2005
Jonathan Tennyson
University College London
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Layers in a star: the Sun
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Spectrum of a hot star: black body-like
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Infra red spectrum of an M-dwarf star
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Cool stellar atmospheres: dominated by molecular absorption
BrownDwarf
M-dwarf
The molecular opacity problem
(m)
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Cool stars: T = 2000 – 4000 KThermodynamics equilibrium, 3-body chemistryC and O combine rapidly to form CO.
M-Dwarfs: Oxygen rich, n(O) > n(C)H2, H2O, TiO, ZrO, etc also grains at lower T
C-stars: Carbon rich, n(C) > n(O) H2, CH4, HCN, C3, HCCH, CS, etc
S-Dwarfs: n(O) = n(C) Rare. H2, FeH, MgH, no polyatomics
Also (primordeal) ‘metal-free’ starsH, H2, He, H, H3
+ only at low T
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Also sub-stellar objects:CO less important
Brown Dwarfs: T ~ 1500 KH2, H2O, CH4
T-Dwarfs: T ~ 1000K‘methane stars’
How common are these?Deuterium burning test using HDO?
Burn D only
No nuclear synthesis
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Modeling the spectra of cool stars
• Spectra very dense – cannot get T from black-body fit.• Synthetic spectra require huge databases > 106 vibration-rotation transitions per triatomic molecule• Sophisticated opacity sampling techniques.• Partition functions also important
Data distributed by R L Kururz (Harvard), seekurucz.harvard.edu
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Physics of molecular opacities:Closed Shell diatomics
CO, H2, CS, etc
Vibration-rotation transitions.
Sparse: ~10,000 transitions
Generally well characterized by lab data and/or theory
(H2 transitions quadrupole only)
HeH+
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Physics of molecular opacities:Open Shell diatomics
TiO, ZrO, FeH, etc
Low-lying excited states.
Electronic-vibration-rotation transitions
Dense: ~10,000,000 transitions (?)
TiO now well understood using mixture of
lab data and theory
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Physics of molecular opacities:Polyatomic molecules
H2O, HCN, H3+, C3, CH4, HCCH, etc
Vibration-rotation transitions
Very dense: 10,000,000 – 100,000,000
Impossible to characterize in the lab
Detailed theoretical calculations
Computed opacities exist for: H2O, HCN, H3+
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Ab initio calculationof rotation-vibrationspectra
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The DVR3D program suite: triatomic vibration-rotation spectraPotential energy
Surface,V(r1,r2,)
Dipole function (r1,r2,)
J Tennyson, MA Kostin, P Barletta, GJ Harris
OL Polyansky, J Ramanlal & NF Zobov
Computer Phys. Comm. 163, 85 (2004).
www.tampa.phys.ucl.ac.uk/ftp/vr/cpc03
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Potentials: Ab initio or Spectroscopically determined
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H3+
H2OH2S
HCN/HNCHeH+
Molecule considered at high accuracy
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Partition functions are important
Model of cool, metal-free magnetic white dwarf WD1247+550 by Pierre Bergeron (Montreal)
Is the partition function of H3+ correct?
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Partition functions are important
Model of WD1247+550 using ab initio H3+ partition function
of Neale & Tennyson (1996)
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HCN opacity, Greg Harris
High accuracy ab initio potential and dipole surfaces Simultaneous treatment of HCN and HNC Vibrational levels up to 18 000 cm-1
Rotational levels up to J=60 Calculations used SG Origin 2000 machine 200,000,000 lines computed Took 16 months
Partition function estimates suggest 93% recovery of opacity at 3000 K
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Ab initio vs. laboratory
HNC bend fundamental (462.7 cm-1).
•Q and R branches visible.
•Slight displacement of vibrational band centre (2.5 cm-1).
•Good agreement between rotational spacing.
•Good agreement in Intensity distribution.
Q branches of hot bands visible.Burkholder et al., J. Mol. Spectrosc. 126, 72 (1987)
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GJ Harris, YV Pavlenko, HRA Jones & J Tennyson, MNRAS, 344, 1107 (2003).
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Importance of water spectra
Other• Models of the Earth’s atmosphere• Major combustion product (remote detection of forest fires,
gas turbine engines)
• Rocket exhaust gases: H2 + ½ O2 H2O (hot) • Lab laser and maser spectra
Astrophysics• Third most abundant molecule in the Universe (after H2 & CO)
• Atmospheres of cool stars• Sunspots• Water masers• Ortho-para interchange timescales
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Sunspots Image from SOHO : 29 March 2001
Molecules on the Sun
T=5760KDiatomicsH2, CO, CH, OH,CN, etc
SunspotsT=3200KH2, H2O,CO, SiO
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Sunspot
lab
Sunspot: N-band spectrum
L Wallace, P Bernath et al, Science, 268, 1155 (1995)
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Assigning a spectrum with 50 lines per cm-1
1. Make ‘trivial’ assignments (ones for which both upper and lower level known experimentally)
2. Unzip spectrum by intensity 6 – 8 % absorption strong lines 4 – 6 % absorption medium 2 – 4 % absorption weak < 2 % absorption grass (but not noise)
3. Variational calculations using ab initio potential Partridge & Schwenke, J. Chem. Phys., 106, 4618 (1997) + adiabatic & non-adiabatic corrections for Born-Oppenheimer approximation
4. Follow branches using ab initio predictions branches are similar transitions defined by
J – Ka = na or J – Kc = nc, n constant
Only strong/medium lines assigned so far
OL Polyansky, NF Zobov, S Viti, J Tennyson, PF Bernath & L Wallace, Science, 277, 346 (1997).
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Sunspot
lab
Assignm
entsSunspot: N-band spectrum
L-band, K-band & H-band spectra also assignedZobov et al, Astrophys. J., 489, L205 (1998); 520, 994 (2000); 577, 496 (2002).
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Assignments using branches
Ab initio potentialLess accurate but extrapolate well
J
Err
or /
cm-1
Determined potentialSpectroscopically
Variational calculations:
Accurate but extrapolate poorly
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ObservedLudwigJorgensen
Miller & Tennyson
Spectrum of M-dwarf star TVLM 513
Water opacities
HRA Jones, S Viti, S Miller, J Tennyson, F Allard & PH Hauschildt (1996)
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Viti & Tennyson computed VT2 linelist:All vibration-rotation levels up to 30,000 cm-1
Giving ~ 7 x 108 transitionsSimilar study by Partridge & Schwenke (PS), NASA AmesNew study by Barber & Tennyson (BT1/BT2)
Computed Water opacity• Variational nuclear motion calculations
• High accuracy potential energy surface
• Ab initio dipole surface
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Spectroscopically determined water potentials
Reference Year vib/cm-1 Nvib Emax /cm-1
Hoy, Mills & Strey 1972 214 25 13000
Carter & Handy 1987 2.42 25 13000
Halonen & Carrington 1988 5.35 54 18000
Jensen 1989 3.22 55 18000
Polyansky et al (PJT1) 1994 0.6 40 18000
Polyansky et al (PJT2) 1996 0.94 63 25000
Partridge & Schwenke 1997 0.33 42 18000
Shirin et al 2003 0.10 106 25000
mportant to treat vibrations and rotations
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Emission spectra of comet 153P/Ikeya-Zhang (C/2002 C1)
N. Dello Russo et al, Icarus, 168, 186 (2004) & Astrophys. J., 621, 537 (2005)Gives rotational temperaturesRotational temperatures & ortho/para ratios
Solarpumping
Emissionlines
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Water in Mira
Cooler than sunspot, but what is T?
vr = 92 km s-1
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NovaV838 MonExplodedFeb 2002
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DPK Banerjee, R.J. Barber, N.K. Ashok & J. Tennyson, Astrophys. J. Lett (submitted).
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Water assignments using variational calculations
• Long pathlength absoption (T = 296K) 9000 - 27000 cm-1
Fourier Transform and Cavity Ring Down
• Laboratory emisson spectra (T =13001800K) 400 – 6000 cm-1
• Absorption in sunspots (T = 3200 K) N band, L band, K band, H band 10-12m 3 m 2 m 1.4 m
30000 new lines assigned
Dataset of 13500 measured H216O energy levels
J. Tennyson, N.F. Zobov, R. Williamson, O.L. Polyansky & P.F. Bernath,J. Phys. Chem. Ref. Data, 30, 735 (2001).
New: lab torch spectra (T ~ 3000 K) from Bernath. 100 000+ lines.
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Bob Barber
Greg Harris
Theoretical Atomic and Molecular Physics and Astrophysics
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Accuracy better than 1cm1 • Adiabatic or Born-Oppenheimer Diagonal Correction (BODC)
• Non-adiabatic corrections for vibration and rotation
• Electronic (kinetic) relativistic effect
• Relativistic Coulomb potential (Breit effect)
• Radiative correction (Lamb shift or qed)
Can BO electronic structure calculations be done this accurately?
Variational rotation-vibration calculations with exact kinetic energy operator accurate to better than 0.001 cm1
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mode Eobs / cm-1 BO +Vad
011 2521.409 0.11 0.24 100 3178.290 1.30 0.40 020 4778.350 0.00 0.50 022 4998.045 0.30 0.64 111 5554.155 1.40 0.50
1 2992.505 1.46 0.36 2 2205.869 0.47 0.25 3 2335.449 +0.47 0.14
1 2736.981 1.04 0.28 2 1968.169 +0.58 0.11 3 2078.430 0.74 0.18
Ab initio vibrational band origins
H2D+
H3+
D2H+
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mode Eobs / cm1 BO +Vad v nuc
011 2521.409 0.11 0.24 +0.056 100 3178.290 1.30 0.40 +0.025 020 4778.350 0.00 0.50 +0.020 022 4998.045 0.30 0.64 +0.010 111 5554.155 1.40 0.50 0.000
1 2992.505 1.46 0.36 0.020 2 2205.869 0.47 0.25 0.050 3 2335.449 +0.47 0.14 +0.090
1 2736.981 1.04 0.28 +0.001 2 1968.169 +0.58 0.11 +0.023 3 2078.430 0.74 0.18 0.004
Ab initio vibrational band origins
H2D+
H3+
D2H+
O.L. Polyansky and J. Tennyson, J. Chem. Phys., 110, 5056 (1999).
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J Ka Kc J Ka Kc Eobs / cm-1 BO +Vad v nuc + KNBO
3 2 1 3 2 2 2225.501 0.385 0.245 0.062 0.044
3 2 1 2 0 2 2448.627 0.521 0.259 0.011 0.076
2 2 0 2 2 1 2208.417 0.435 0.242 0.050 0.068
2 2 1 2 0 2 2283.810 0.521 0.239 +0.030 0.059
2 2 0 1 0 1 2381.367 0.573 0.250 +0.008 0.060
3 3 1 2 1 2 2512.598 0.647 0.250 +0.075 0.099
2 0 2 3 1 3 2223.706 0.418 0.163 +0.050 +0.068
2 2 1 3 1 2 2242.303 0.753 0.151 +0.140 +0.095
2 1 2 2 2 1 2272.395 0.420 0.168 +0.035 +0.099
2 2 0 2 1 1 2393.633 0.320 0.162 +0.140 +0.087
3 3 1 3 2 2 2466.041 0.224 0.164 +0.190 +0.080
3 3 1 2 2 0 2596.960 0.185 0.177 +0.167 +0.077
3 3 0 2 2 1 2602.146 0.203 0.172 +0.167 +0.080
2
3
H2D+ : ab initio spectra
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Obs / cm1 5Z1 6Z1 CBS2 CBS+CV3
(010) 1594.75 2.99 2.30 0.32 +0.48 (020) 3155.85 4.22 2.38 0.79 +1.16(030) 4666.73 6.30 3.24 1.52 +2.05(040) 6134.01 9.81 5.54 2.74 +3.20(050) 7542.44 14.70 9.19 4.72 +4.82 (101) 7249.82 +12.51 +10.76 +9.32 5.35 (201) 10613.35 +18.72 +16.46 +13.97 7.47(301) 13830.94 +25.72 +22.81 +18.74 8.97 (401) 13805.22 +32.56 +28.92 +23.06 10.17(501) 19781.10 +40.72 +35.96 +28.68 10.72[104]all 22.84 19.74 16.567.85
Ab initio calculations for water
1 MRCI calculation with Dunning’s aug-cc-pVnZ basis set2 Extrapolation to Complete Basis Set (CBS) limit3 Core—Valence (CV) correction
OL Polyansky, AG Csaszar, J Tennyson, P Barletta, SV Shirin, NF Zobov, DW Schwenke & PJ KnowlesScience, 299, 539 (2003)
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BO / cm1 +BODC1 + Non-adiabatic
v nuc2 diag3 full4
(010) 1597.60 0.46 0.19 0.06 0.07 (020) 3157.14 0.94 0.38 0.12 0.15(100) 3661.00 0.55 0.46 0.72 0.70 (030) 4674.88 1.43 0.55 0.18 0.23(110) 5241.83 0.16 0.65 0.77 0.76 (040) 6144.64 2.00 0.71 0.23 0.30(120) 6784.56 0.23 0.83 0.83 0.84(200) 7208.80 1.25 0.88 1.39 1.37 (002) 7450.86 1.47 0.90 1.47 1.57(050) 7555.62 2.71 0.84 0.28 0.32
Born-Oppenheimer corrections for water
1 Born-Oppenheimer diagonal correction using CASSCF wavefunction2 Non-adiabatic correction by scaling vibrational mass, V
3 Two parameter diagonal correction4 Full treatment by Schwenke (J. Phys. Chem. A, 105, 2352 (2001).)
J. Tennyson, P. Barletta, M.A. Kostin, N.F.Zobov, and O.L. Polyansky, Spectrachimica Acta A, 58, 663 (2002).
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Ab initio predictions of water levelsIsotopomer N(levels) J(max) / cm
H216O 9426 20 1.17
H217O 669 12 0.28
H218O 2460 12 0.65
D216O 2807 12 0.71
HD16O 1976 12 0.47All water 17338 20 0.95
Rotational non-adiabatic effects very important
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Residual sources of error
• Basis set convergence of MRCI:
need extrapolated 7Z• Full CI: contributes ~ 1 cm at 25,000 cm (?)• Surface fitting: 346 points computed,
need 1000 points, reduce by ~ 0.2 cm
• Full inclusion of non-adiabatic effects
up to 25,000 cm-1