1. Stratospheric and Mesospheric Applications of SCIAMACHY Limb Observations C. von Savigny, A. Rozanov, G. Rohen, K.-U. Eichmann, E. J. Llewellyn *, J. W. Kaiser +, M. Sinnhuber, M. Scharringhausen, P. Ulasi, H. Bovensmann, and J. P. Burrows Institute of Environmental Physics/Remote Sensing, University of Bremen, Bremen, Germany * Department of Physics and Physics Engineering, University of Saskatchewan, Saskatoon, Canada + Remote Sensing Laboratories, University of Zurich, Zurich, Switzerland 5th German SCIAMACHY Validation Team Meeting

2. Stratospheric applications –Polar stratospheric clouds –Minor constituent profiles Mesospheric applications –Mesospheric ozone profiles –OH * (3-1) rotational temperature retrievals –Noctilucent clouds Outline

3. SCIAMACHY Limb Geometry Tangent height range: 0 to 100 km Tangent height step size: 3.3 km Vertical FOV: 2.6 km Observation optimised for limb-nadir matching Duration of Limb sequence: 60 s Observed is limb scattered solar radiation and terrestrial airglow emissions On the Earth’s night side limb emissions are observed in a dedicated mesosphere / thermosphere observation mode with tangent height between 75 and 150 km. Illustration of the limb-scattering geometry

4. Polar Stratospheric Clouds

5. Step I: Determine colour index profiles Step II: Determine vertical gradient of CI(TH): with  TH = 3.3 km Theoretical maximum  (TH) values for 15-30 km altitude range: a) 1.05 for pure Rayleigh atmosphere b) 1.1 for stratospheric background aerosol c) 1.16 for moderate volcanic aerosol d) 1.55 for extreme volcanic aerosol Detection threshold chosen:  (TH) = 1.3 detection is somewhat biased towards optically thicker PSCs PSC detection with limb measurements

6. Maps of detected PSCs (open circles: detected PSCs) superimposed to UKMO temperature field at 550 K potential temperature (about 22 km) for August 7-12, 2003. PSC maps

7. 190 195 190 195 190 No SCIAMACHY Observations No SCIAMACHY Observations No SCIAMACHY Observations Temporal variation of PSC altitudes PSC descent rates for 2003: Santacesaria et al. [2001] : 2.5 km / monthat 66º S / 140º E based on a 9-year Lidar climatology Fromm et al. [1997] :2.0 km / month derived from POAM II 50º S - 60º S2.5 km / month 60º S - 70º S2.0 km / month 70º S - 80º S1.2 km / month

8. Histograms of temperature at PSC altitude

9. Stratospheric Minor Constituents

10. The scia-arc website The scia-arc website provides value-added scientific data products Presently available limb data products: stratospheric profiles of O 3, NO 2 and BrO In preparation: - mesospheric O 3 profiles - maps of NLCs and PSCs - OH rotational temperatures at the mesopause http://www.iup.physik.uni-bremen.de/scia-arc

11. One week before the major stratospheric warming: September 12, 2002 Savigny et al. [2004]

12. The ozone hole split: September 27, 2002

13. At mid-latitudes typical BrO mixing ratios are about 10 pptv, corresponding to about 50 % of the available inorganic bromine (20 pptv). The rest is almost exclusively BrONO 2.[e.g., Sinnhuber et al., 2002] Within the vortex BrO mixing ratios are most likely enhanced due to the reduced NO 2, therefore reduced formation of BrONO 2.

14. OH rotational temperature retrievals

15. OH* produced and vibrationally-rotationally excited at mesopause altitudes by: H + O 3  OH* (v’  9) + O 2 + 3.3 eV Airglow emission centered around 87 km with about 8 km FWHM Relative population of rotational levels governed by Boltzmann’s distribution Measurements of relative intensities of rotational emission lines makes retrieval of OH rotational temperature possible OH*(v’ = 3) is in local thermodynamical equilibrium (LTE) for lower rotational quantum numbers because: - collisional frequency at 86 km is 3  10 4 s -1 - lifetime of OH at v’ = 3 is about 0.014 s rotational temperatures are equal to kinetic temperature of ambient air Retrieval of OH* (3-1) rotational temperatures

16. E J  J(J+1) J’=0 J’=2 J’=3 J’=4 J’=5 Selection rule:  J = 0,+1,-1 ’=3 ’’=1 P-branch  J = + 1 Q-branch  J = 0 R-branch  J = -1 J’=1 J’’=0 J’’=2 J’’=3 J’’=4 J’’=5 J’’=1 Q-branchP-branch

17. Impact of different Einstein coefficients used: Kovacs [1969], Mies [1974], Goldman et al. [1998] T Kovacs – T Mies = 1.1 K and T Kovacs – T Goldman = 3.2 K Sample OH spectral fit Iterative retrieval approach: (1)linear fit with 2nd order polynomial (2) non-linear fit (Levenberg-Marquard) driving OH model, including -shift

18. Calibration measurements Calibration measurements Limb measurements Limb measurements Calibration measurements Coverage of Limb eclipse measurements

19. Replacement of nighttime Nadir observations by limb observations Implemented on September 6, 2004 SCIAMACHY Operations Change Request 19

20. GRound-based Infrared P-branch Spectrometer (GRIPS) I at Hohenpeissenberg (47° N / 11° E) GRIPS-I data provided by Michael Bittner and Kathrin Höppner (DLR) First validation results Mesospheric Temperature Mapper (MTM) at Hawaii (21° N / 204° E) MTM data provided by Mike Taylor and Yucheng Zhao (Utah State University)

21. OH-Temperatures 2003 Temperatures: for latitudes from –20 to 70 deg from July 2002 up to now.

22. Mesospheric Ozone

23. Weighting functions Averaging kernels

24. Ozone depletion during the Oct. / Nov. 2003 SPEs HO x production by ionization: O 2 + + O 2 + M  O 2 +O 2 + M O 2 +O 2 + H 2 O  O 2 +H 2 O + O 2 O 2 +H 2 O + H 2 O  H 3 O + OH + O 2 H 3 O + OH + H 2 O  H 3 O + H 2 O + OH H 3 O + H 2 O + e -  2 H 2 O + H O 2 + + H 2 O + e -  O 2 + H + OH (Courtesy M.-B. Kallenrode and M. Sinnhuber ) NO x is formed as well

25. Ozone depletion during the Oct. / Nov. 2003 SPEs Ozone loss at 55 km and north of magnetic 60° N relative to October 20 – 24 reference period 40 MeV protons penetrate the atmosphere Down to about 45 km altitude

26. Observations vs. Model SCIAMACHY measurements Model simulations (M. Sinnhuber) Percent ozone loss north of 60° N magnetic latitude Reference period: October 20 – 24, 2003

27. Noctilucent Clouds

28. UV limb radiance profiles with NLCs and without NLCs Detection of Noctilucent Clouds (NLCs)

29. I. In single scattering approximation the PMC backscatter is given by: q(,  ): Differential scattering cross section S( ): Solar irradiance spectrum II. The sun-normalized PMC backscatter spectrum: with spectral exponent  NLC particle size determination I

30. Ambiguity: spectral exponent does not monotonically increase with increasing radius Use several and significantly different wavelengths to determine r and  [von Cossart et al, 1999]. Assumptions: Mie theory, i.e., homogeneous dielectric spheres Refractive index of ice [Warren, 1984] Log-normal distribution The spectral exponent  is related to the PMC particle sizes by Mie-calculations Simulated spectral exponents  for log- normal distribution with  = 1.4 NLC particle size determination II

31. NLC particle size determination – January 2003

32. Conclusions SCIAMACHY limb observations with their broad spectral coverage and extended altitude range both on the day and nightside allows a wide range of stratospheric and mesospheric to be studied: Optically thin aerosols like NLCs and PSCs Minor constituent profiles (O 3, NO 2, BrO; soon H 2 O, CH 4 ) Mesopause temperature (soon Rayeigh temperatures)