Middle atmosphere temperatures were measured during the MAP/WINE campaign by various ground-based techniques, by rocket instruments, and by satellites. Respective data were analyzed for atmospheric thermal mean state as well as for long and short period variations. A brief survey of the results is given. Monthly mean temperatures agree well with the new CIRA model. Long period (planetary) waves frequently exhibit peculiar vertical amplitude and phase structures, resembling those of standing waves. Short period oscillations tend to begin breaking well below the stratosphere

Offermann, D.

English

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237
7.3 MIDDLE ATMOSPHERE THERMAL STRUCTURE DURING MAP/WINE
D. Offermann
Physics Department, University of Wuppertal
5600 Wuppertal 1
Federal Republic of Germany
Middle atmosphere temperatures were measured during the MAP/WINE campaign by
various ground-based techniques, by rocket instruments, and by satellites. Respective data
have been analyzed for atmospheric thermal mean state as well as for long and short period
variations. A brief survey of the results is given. Monthly mean temperatures agree well with
the new CIRA model. Long period (planetary) waves frequently exhibit peculiar vertical
amplitude and phase structures, resembling those of standing waves. Short period oscillations
tend to begin breaking well below the stratosphere.
Temperature Measurements during MAP/WINE
Technique Place/In stitution
1. Ground-based
Lidar
Lidar
Near infrared
OH spectrometers
OH spectrometers
OH spectrometer
Observatoire de Haute Provence/CNRS
Andoya/Bonn University
Andoya/Wuppertal University
ESRANGF_A.Itah State University
Lista, Oslo/Wuppertal University; NDRE
Zvenigorod/IPA
2. Rockets
Met. rockets
Datasondes
Falling spheres (passive)
Falling spheres (active)
IR radiometers
Mass spectrometers
IR spectrometer
Datasondes
Met. rockets
Heiss Island/CAO
Andoya/Bonn University
Andoya/Bonn University; NASA GSFC
Andoya/AFGL
Andoya/Wuppertal University
Andoya/Bonn University
ESRANGFJWuppertal University
Lista/NASA GSFC; NDRE
Volgograd/CAO
3. Satellites
Stratospheric Sounding Unit
SSU
NOAA
Figure 1. Techniques used for middle atmosphere temperature measurements during
MAP/WINE. For details see the following papers in J. Atmos. Terr. Phys., 49, 1987: v.
Zahn, p. 607; Petzold et al., p. 621; Hauchecorne et al., p. 649; Offermann et al, p. 655; v.
Zahn, p. 863. Also, Schmidlin, ESA SP 270 (Sunne), 133, 1987; Gerndt, Ph.D., University
of Wuppertal, 1986; Briickelmann, Ph.D. University of Wuppertal, 1988; Meyer et al., ESA
SP 229 (Loen), 41, 1985; Liibken et al., ESA SP 229 (Loen) 259, 1985.
https://ntrs.nasa.gov/search.jsp?R=19890020518 2020-03-20T00:40:58+00:00Z
238
E
oJ
.-I
4--
<_
95
90
85
8o
75
70
65
60
55
50
45
40
35
30
25
20
15
-- rocket dnfa
.... Barnett and Corney (1985)
..... Groves (198S)
_. Jan. 1984
lllllllllllllllllllllllllllllllt +[llllJllllJllll|lllll 111111111Jllll
, +
180 200 220 240 260 280 300
Temperature [K]
Figure 2. Mean temperature pmf'fle calculated from the rocket measurements above Andoya in
January 1984. The model profiles of Barnett and Comey (Handbook for MAP 16, 47, 1985)
and Groves (AFGL-TR-85-0129) are given for comparison. Differences between measured
and model profiles in the mesosphere appear to show a precursor structure related to the major
stratospheric warming, which occurred by end of February 1984. (For details see Offermann
et al., J. Atmos. Terr. Phys., 49, 655, 1987.)
239
9O
8O
8Skin m
+ +
SO
3O
15 1 15 _11 15
December 1983 Jonuory1981, Februory 198/,
Figure 3. Harmonic least square fit to temperatures measured at given altitudes during the
MAP/WINE campaign above Andoya. Analysis is performed at 1 km altitude steps, only part
of which is shown here. Five oscillations are superimposed. The periods are 9.6 days, 13.3
days, 17.4 days, 54 days and 144 days. The shorter ones are believed to represent planetary
waves (Details of this and the following pictures are given by Offermann et al., d. Atmos.
Terr. Phys., 49, 655, 1987.)
240
2
70
60
SO
40
3O
80
70
<
50
40
30
28kin
I I
15 1 '15 1 '15
December1983. Jonuory 1984 Februory 1984
86 km
:15 '1 '15 '1 '15
December1983 January 1984 February 198_
Figure 4. Two components of the harmonic analysis shown in Figure 3 (Andoya): a) period is
9.6 days, b) period is 13.3 days.
-3
90,
80
7O
m
50-
40:-
Phase {tad!
-2 -1 0 1 2 3
30 ¸
2O
0
///
Amptitude[K]
90 / I I I 1/ I •
801"'---"_ ( 1010211984
I ' I I |
O_ 1 2 io
Volumemixingrat_ [ppn_]
241
Figure 5. Vertical amplitude and phase structure
of the wave with 13.3 days period. Oscillation
nodes with amplitude minima and phase jumps
(of about 180°) are seen at altitudes of 46kin
and 76 kin. They are indicative of a standing
wave. Similar structures are seen in most of
theotheroscillations analyzed. They were
alsofoundinotherwintercampaignsin
Western Europe.
Figure 6. Ozone mixing ratios as measured by
infrared rocket experiments (at night). Dashed
line is a very approximate mean curve including
several other measurements. With respect to
this curve, ozone is found to be depleted above
76 kin, and enhanced below this level. The
levelcoincideswithone ofthenodesofthe
13.3d oscillation(Figure5).Only a small
fractionoftheozonedeviationscan bc
explainedby photochemistry.(Fordetailssee
Grossmann etal.,J.Atmos. Terr.Phys.,49,
827, 1987.)
242
"o
90"
8O
7O
60'
50
( \ SME,10.2.198_,
J ', 6-y
. ," --70 N, 37 E
f SS_ ._ J i
\x, _
o11 i i
Votume mixing rnl'io [ppmv]
lO
Figure 7. Ozone mixing ratios as measured by
the SME satellite at two different longitude=.
Measurements are during daytime. Dashed
curve is at 378 east and resembles quali-
tatively the solid curve in Figure 6. Hence
the wave structure extended to this longitude
at least. The profile at 68 west resembles an
undisturbed profile, i.e., a wave with zero
phase. If it is assumed that the dashed curve
approximately shows the maximum of the
wave disturbance, and the solid curve shows
zero disturbance, a longitudinal wavelength
of 428 results. Hence the disturbance seen is
compatible with a planetary wave 2. A similar
result was obtained before by Hauchccom¢ et
al. [1987] (s¢¢ Figure 8).
UOLGO(;RAO / OHP
I i90
E
=8o
50 _ r •
_0 i: ':'._... ", "_
30 _
0.01 0,03 0.05
OATS-_
TE_PER^TURE SPECTRUM
I I I
, ,=,"<z_:> ,=
q • & ¢
o • _ '¢
I , I
0.03 0.09
d ¸
•*- 25
. 50
";5
, 100
Figure 8. Fourier analysis of temperature measured by lidar and rockets at the Observatoire de
Haute Provence (OHP) and at Volgograd, respectively (Hauchecorne et al., J. Atmos. Terr.
Phys., 49, 649, 1987). Direction of the arrows gwes the phase difference between the two
stations. An arrow directed toward right indicates that the maximum occurs sooner at OHP
than at Volgograd. The wave at 12.5 days period (45 km, 70 km) shows westward
propagation and is interpreted as a planetary wave 2 (second symmetric mode).
243
P
:= 60
30
o I1 '1'15 '15
December1983 January 1984 February 1984
Figure 9. Comparison of an oscillation with 13.3 days period at Andoya (solid lines) and
OHP (dashed lines). The lidar data of OHP were analyzed by the same technique as sketched
for Andoya above (Figures 3 - 5). An oscillation period of 12.5 days was obtained which is
exactly the same as the one of the Fourier analysis of Hauchecome et ai. [1987]. When a
period of 13.3 days is prescribed to the OHP data (this picture), an anticorrelation between
Andoya and OHP is obtained above the node at 46 km, and a phase shift greater than 908 in
most part below it.
17.i.0
30_0 20 m- " -- _" -- - _" ' "
o1' '15 '1 '15 '1 'lS
December1983 January 1984 February 198/,
Figure 10. Comparison of an oscillation with 9.6 days period at Andoya (solid lines) and
OHP (dashed lines), the 9.6 day value is prescribed to the OHP data. An anticorrelation
between the two stations is obtained in most part of the altitude regime, except around the
node at 48 km (arrow) and the very lowest altitudes. Please note that a phase reversal occurs at
the node (Andoya) similar to and even larger than the one shown in Figure 5 at 46 km.
244
Wave Summary
Periods observed: 12.5 d - 13.3 d 9.6 d
Vertical structure:
kz/2: - 30 km - 30km
Nodes at: 46 kin, 76 km 48 km, 76 km
Zonal structure:
_tx 180 ° (wave 2) ?
Meridional structure:
Nodes at 50°-60°(7) 50°-60° (7)
Figure 11. Results obtained from rocket data at Andoya and lidar data at OHP for the two
shortest oscillation periods. Meridional structure results are preliminary. Respective analysis
is still inprogress.
9O
a.)
8O
7O
20
RJ ¢0
... , ..... , #
10% 20% 30%
Io.) c.)
\
O,Ri¢¼ _,Ri¢1
.. , g , . , .... , .... , -.
0 10%0 10% 20% 30%
Figure12. OccurrencefrequencyofRichardsonnumbers R iatAndoya asdeterminedfrom
more than60 rocketflightsduringthreemonths. Atmosphericinstabilitysetsinaslow as35
krn.Above thisaltitudetheatmosphereisunstable(Ri< I)formore than50% ofthetime.


Middle atmosphere thermal structure during MAP/WINE

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