1. Large-eddy simulation of an observed evening transition boundary layer
Here is a nice picture of a stable bl in California.
Dr Bob Beare
John M Edwards and Alan Lapworth
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2. Aims
Establish if LES of the evening transition is possible. Nieuwstadt and Brost 86 and Sorbjan 97 look at decay of convective turbulence but not full transtion. Domain size for CBL (>2-4km in horizontal) and grid length requirements for SBL (1-10 m).
Comparison with surface and tethered balloon measurements.
Three types of run: full transition (CBL-SBL), nocturnal development (just SBL, smaller domain), degraded resolution (just SBL).
See Beare et al 2005, to appear in QJRMS.
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3. Cardington observations
Reasonably flat grassy site, z0m = z0h = 5 cm near Bedford UK.
Times series of 1.2 m temp., 4 m sensible heat flux and friction velocity.
Tethered balloon observations for transitions 7-8 April and September 2003 (clear skies, moderate gradient winds ~ 7m/s, moderately stable: h/L~2-4), every hour after sunset. Sept case had significant nocturnal jet and inertial oscillation, thus focus of study.
See Lapworth and Mason (1988) and Lapworth (2003) for more info about site and obs method.
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4. Large-eddy simulation (LES) model
Full transition run: 12Z – 0Z; 2km x 2km x 3km domain; 10 m grid length. Mainly temperature boundary conditions (some flux).
Smagorinsky diffusion (blue) ; Stochastic backscatter (red), Brown et al. (1994).
Zero moisture; radiation code off (approximated by constant interior cooling forcing).
Temperature bottom boundary condition for other runs; grid length typically 5m; 500mx500mx1km domain.
LES equations: momentum, heat ,continuity
dry, advection, coriolis, p-grad, buoyancy,
SUB-GRID model…
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5. Full transition: surface parameters
Area averaged u* and SHF (hence smoother) vs surface obs. Sunset ~ 18Z
Similar mag in CBL, but delayed decay. Over prediction of u*, and SHF in SBL phase (a bit like large scale models).
Slightly better timing with flux bcs.
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6. Full transition: flux profiles, every hour from 19Z
Full transition: flux profiles, every hour from 19Z. Buoyancy and TKE fluxes.
Normalise buoyancy and TKE flux after transition.
Curvature of wb going from curved to linear. cf obs of Grant 97.
Collapse of TKE flux; quite suddenly collapse.
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7. Mean profiles. Observations thick dashed lines.
Analytical initialiastion
Full transition
Full transition runin early eve. has too shallow a SBL and too weak ageostrophic wind… A problem
(uncertainty in intial profile (from mes) or poor simulation of the collapse of the bl)
So to make progress with comparing LES with obs for the SBL, we had to reinitialise with an analytic fit to obs.
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8. Comparison of LES and tethered balloon observations for Cardington, Bedford; nocturnal development
LES area averaged. Captures positive curvature and jet. Differences low down (decoupling?)
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9. Sensitivity to initial wind profile; nocturnal development
Sensitivity to initial conditions. Jet all but disappears with geostrophic initialisation.
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10. Nocturnal development: sensitivity to forcings and model
Sensitivity to forcings bigger than that for the model. Although double resolution pushes solution further away from obs.can’t say with
conviction that this is a worse simulation as forcings are uncertain.
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11. April 2003 case Very good match in theta; no low level jet in OBS.
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12. Grid length: 1000m in horizontal, 100m in vertical
Cardington case: sensitivity to stability function; degraded resolution runs
Grid length: 1000m in horizontal, 100m in vertical
SGS model providing all the fluxes; SHARP is control ; long tails like large-scale models
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13. Vertical velocity cross-section and spectra
Distinct peak
Red positive, blue down
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14. Momentum budget (Sept 2003 case, 0230Z)
Momentum budget indicating significant inertial oscillation above SBL.
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15. Summary
LES of evening transition is possible (although robustness not fully explored due to computational burden) and qualitatively correct. Significant differences between model and obs in details: ageostrophic wind and collapse of the CBL stress (cf Mahrt 1981, for Wangara).
Good comparison for nocturnal development runs, initialised with obs in early evening.
Uncertainties in the geostrophic, surface and radiative forcings can make detailed comparison difficult and hard to say which model configuration is better.
Nesting may be helpful for full transition at higher resolution.
© Crown copyright 2004