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Table 1. Characteristcs of wind profilers of WINDAS.AFrequency1357.5 MHzAntennacoaxial colinear arrays with gainof 33dB and size of 4m x 4mPeak Power 1.8 kWBeam width 4 deg.Beam configuration 5 beamsPulse length 0.67, 1.33, 2.00, 4.00 10 -6 sec.PRF5, 10, 15, 20 kHzSide robe level -40dB or -60dB(at elevation angles of 0-10deg)Basic dataDoppler moments every 1minuteDistributed data U,V,W-components of wind,S/N ratio & data quality flag every 10 minutesPressure(hPa)4005006007008009001000WPR (June)TMP (June)WPR (July )TMP (July )0 1 2 3 4 5 6Figure 3. Vertical distributions of RMSEs of profilerwinds (WPR) from winds RMSE(m/s) by mesoscale model(MSM)and those of radiosondes winds (TMP).u-components of winds in June and July 2001 areexamined.HEIGHT(m)9000TotalNonprecipitationUnder precipitation800070006000500040003000200010000J UNE JULY AUG. SEP. OCT. NOV. DEC. JAN. FEB. MAR. APRIL2001 2002Figure2. Monthly total means of height coverage for 25 wind profilers of WINDAS.(a) (b) (c)135ERR130EWWRRWRWWWWWWWR3-hour rainfall amount (mm)100kmFigure 4. Result of an observing system experiment on comparison between forecasts by the mesoscale model (MSM)and observations for 3-hour rainfall amount. The initial time is 12UTC on 19 June 2001. (a) forecasts from MSM and 4D-VAR without profiler data but radiosonde data, (b) forecasts from MSM and 4D-VAR with both profiler data andradiosonde data, and (c) rainfall amount observed by radars and rain gauges during 12 to 15UTC. ‘R’s in (a) and (b)indicate the locations of the radiosonde sites and ‘W’s in (b) the locations of the wind profiler sites.356
FIRST RESULTS OF THE BOUNDARY LAYER AND TROPOSPHERICRADAR SYSTEMS FOR ENSO STUDIES IN NORTHERN PERUD. Scipión 1 , J. Chau 1 , and L. Flores 21 Radio Observatorio de Jicamarca, Instituto Geofísico del Perú, Lima2 Laboratorio de Física – Universidad de Piura1. Introduction.The Instituto Geofísico del Perú (IGP) has recently bought with the cooperation of theWorld Bank, two new Boundary Layer & Troposphere Radar (BLTR) systems to improve thecapacity for predicting and evaluating the El Niño phenomenon (ENSO) to assist in theprevention and mitigation of disasters in Peru (R. Woodman and P. Lagos, personalcommunication). Both systems have been installed in northern Peru, because this area is one ofthe most sensitive to El Niño phenomenon in the World. In particular, Piura which is a desertlikearea with an average annual rainfall of 50 mm, in few months of ENSO becomes a tropicalarea (rainfall of 3000 mm in less than 6 months!). The data from these systems will beincorporated to the regional numerical weather model of IGP.The first system was installed at Universidad de Piura (UDEP) where it complementsthe existing Piura ST system [Gage et al., 1991]. As we will show below, the validation of thenewly installed BLTR system in Piura has been tested against winds obtained wit the ST radarand also against winds obtained from pilot balloons. The ST and BLTR radars operate at49.920 MHz, and we avoid possible interference between both of them by operating the BLTRsystem in slave mode. The second BLTR system was installed ~200 km SE of Piura close toPorcuya. Atmospheric dynamics above this site will be very important because it is located atthe lowest part of the Andes in the northern part of Peru and therefore in the border of thePacific and Atlantic basins.In this work, we will present first results, comparison and statistical studies betweenBLTR, ST and Pilot Balloons of instantaneous data, consensus data, and NCEP Reanalysis dataover UDEP and Porcuya.2. Peruvian ProfilersTable 1 shows the different systems operating in Northern Peru. The ST system wasinstalled in 1989 as part of the Transpacific Profiler Network [e.g., Gage et al., 1991], itoperates at 49.92 MHz and uses the Doppler Beam Swinging (DBS) technique; its rangecoverage is between 2 – 12kms. with 1km resolution and it takes 12 minutes to cover all thebeams (north, south, east, west and vertical).Table 1 Wind profilers in Northern Peru.Location Altitude Type Band Size Peak Power Method PeriodPiura 43m. ST VHF 100m x 100m 30 kW DBS 1989 -Piura 43m. BLT VHF 30m x 30m 12 kW SA 2001 - ?Porcuya 1163m. BLT VHF 30m x 30m 12 kW SA 2002 -357
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MST10Tenth InternationalWORKSHOPOn
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MST 10 Group PictureMay 15 th , 200
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TENTH INTERNATIONAL WORKSHOP ON TEC
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Table of ContentsPREFACE ..........
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I.2.18 FURTHER OBSERVATIONS OF PMSE
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I.3.27 NEW MST RADAR METHODS FOR ME
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I.4.19 STUDY OF A MESOSCALE LAND-TO
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I.5.502 AN ATTEMPT TO CALIBRATE THE
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PrefaceMST10The Tenth International
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and the local organizing committee,
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The operational aspects and recent
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To improve the understanding of dyn
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Improving MST radar resolution by u
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latitudes, arguing that the former
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Report on Session I.3 “Winds, Wav
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Turbulence.The session then moved i
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Report on Session I.4 “Meteorolog
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Multiple Antenna Profiling Radar (M
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Report on Session II “Novel Persp
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synchronized by GPS and connected v
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The highly positive response of the
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10th International Workshop on Tech
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10th International Workshop on Tech
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Session I.1: Radar scattering proce
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⎡7800 ∂q⎤(3)⎢ 15500q⎥M =
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Figure 2 compares profiles of ω B
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Figure 1: Data from the MST radar a
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Ri =shear2ωB22⎛ ∂u⎞ ⎛ ∂v
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Meridional (deg)1050−5−10Echo P
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Subarray Configuration, Capon Metho
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Fig. 2 PMSE plot (SOUSY Svalbard Ra
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VHF radar interferometry had shown
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turbulence. From Figures 1 and 2, i
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SummaryFrom the aspect sensitivity
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a specific range. In this work, syn
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P C(dB)(a) Echo Power60504030200.70
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most occidental area of South Ameri
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Quegan, 1992). It should be useful
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measurements, is shown in figure 1(
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The present observations thus empha
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RECENT OBSERVATIONS OF E REGION FIE
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measured spectra in order to separa
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drifts at E and F regions heights b
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• Are characterized by type II ec
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The main parameters that could be o
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THE ROLE OF UNSTABLE SPORADIC-E LAY
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(σ H / σ P )E y (where σ H and
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STUDY OF A LOW E-REGION QUASI-PERIO
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100 m/syrFigure 4: Geometry of the
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Where the notations carry same mean
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Where dx/dt and dy/dt are the veloc
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non-negativity of the image is prio
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spectrum corresponding to the backs
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The Artigas and Machu-Picchu Statio
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Arguments against the second altern
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Extension of the Kolmogorov spectru
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volumeESRvolumeSSRSSR SSRESR ESRSSR
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individual particles in a statistic
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Anomalous spectraTalkner [4] studie
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To observe the E region FAI echoes,
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matter daytime or nighttime and are
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two sub-arrays, each sub-array made
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4. SummaryHere we describe a radio
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Figure 1. E-region DPS4 spectra, ri
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effects. It is therefore plausible
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1996 and high in 2002). The electri
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electric fields map along the geoma
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SNR condition is always difficult a
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Figure-4 Power spectrum plots of a
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As we show below, Jicamarca offers
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particularly during daytime counter
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where ˆδ nm = (δ l − δ m )
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PMSE is more easily interpreted as
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ResultsTemperature climatology• s
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Simultaneous PMSE and NLC observati
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ResultsSeasonal variationMSE are no
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Figure 2: MSE parameters as functio
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Session I.3: Winds, waves and turbu
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poor. It was shown that poor perfor
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The use of diffraction pattern simi
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F 13 (ξ x ′) = (1 − cos 2ψ N)
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Figure 3: (a) Baseline length depen
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3. ResultsFigure 1 shows the amplit
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variability.Figure 4 shows the aver
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Figure 1. Period-time amplitude wav
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the 12-h and 24-h periodicities in
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winds and variances at altitudes 70
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similar correlation with larger mag
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of the refraction index are not equ
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Fig. 8. Zonal wind (top) and temper
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STUDIES ON ATMOSPHERIC GRAVITY WAVE
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1100-1200 hours. From this plot 6.3
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STUDIES ON WINDS AND MOMENTUM FLUXE
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3.4 Monthly variation of momentum f
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DEEP PENETRATIVE CONVECTION AND GEN
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ly changes direction with time with
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189
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191
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193
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These two last relations are the on
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3.2.1 From v ′2 to ɛ kThe questi
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5.2 Frequency distributionsSeveral
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ReferencesAlisse J.-R. and C. Sidi.
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Röttger J. and C.H. Liu. Partial r
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Specular reflection is negligible f
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−0.5C n2 Distribution (PROUST & S
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the beamwidth, α is the zenith ang
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this latitude in late April). Surfa
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Fig. 1. Median (upper) winds and (l
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Fig.1. Lines of constant radial vel
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which have not yet been considered
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is calculated from the radiosonde t
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Figure 3: Time-altitude cross-secti
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Absorption of cosmic noise is cause
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Incoherent scatter spectracompared
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variations of spectral widths, refr
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Figure 1. Diurnal variation of Turb
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further experimental test of the ST
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waves can be observed more clearly
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winter and a minimum in summer near
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The main recently assumed mechanism
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Figure 2. Statistics of numbers of
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LIDAR OBSERVATIONS OF MIDDLE ATMOSP
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latitudinal dependence of the seaso
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APPLICATION OF THE DUAL-BEAMWIDTH M
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Figure 2: Mean zonal and meridional
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JLKLLK/ILIL6II/G/II/G/LEODFLK/LO/DD
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The monthly diurnal mean of horizon
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Session I.4: Meteorological Phenome
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Integration of the VHF wind profile
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Figure 1 : Map of the Lago Maggiore
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precipitating clouds, the cyclonic
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Eyewall(a)(b)(c)(d)Fig. 3: Radius-h
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as low as 0.55. The Piura 50-MHz ra
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place features in the profile with
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• Period 1 (June 1-10): SCCs exis
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Sumatera occurs by stratiform cloud
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very interesting to note the double
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20(a) Convective Region(b) Transiti
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Typhoon LekimaFig. 2 Typhoon Lekima
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Fig. 5 Passage of typhoon Hayan on
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the 50 cm 2 sensor head, enabling t
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22 June 2000 23:22:23 - 23:24:20 at
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the time-height section of a convec
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Thurai, M., T.Iguchi,T. Kozu, J.D.E
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There are two main mechanisms which
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Horel, J.D. and Cornejo-Garrido, A.
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estimating two independent and redu
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RASS THETA (K) RASS v-component (m/
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Surface winds usually range from 10
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weak (maximum of 5 m s -1 ) and the
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The vertical component from the VTB
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Figure 8 shows the profile of virtu
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2 3D ( , ) ( ) ( ) ˆ ( ) ˆp∆ xm
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Page 313 and 314: In Fig. 2 a sketch of a mountain le
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Page 333 and 334: Histogram of Zonal Velocityh=5.13 K
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Page 339 and 340: Boundary layer height, km32.521.5(a
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Page 345 and 346: 3. Results and discussionIn the pre
Page 347 and 348: 4. SummaryAn attempt has been made
Page 349 and 350: The purpose of this study is to exa
Page 351 and 352: Figure1. Three-day average of momen
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Page 355 and 356: But in case of period until 1800 UT
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Page 359 and 360: The profilers of WINDAS weredesigne
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Page 373 and 374: 3. Cloud Evolution Case StudyOn the
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Page 377 and 378: Experiment 1 Experiment 2IPP 999Km
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Page 381 and 382: The main element of the unit (figur
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Page 389 and 390: Table 2: Experiment #1 results, Tra
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Page 393 and 394: Off-zenith beams towards N, S, E, W
Page 395 and 396: 95ALWIN VHF radar: signal powerdB80
Page 397 and 398: ANTENNA BEAM VERIFICATION USING COS
Page 399 and 400: Figure 2: A 45 MHz reference sky te
Page 401 and 402: AN ATTEMPT TO CALIBRATE THE UHF STR
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Page 405 and 406: QUALITY CONTROL FOR DOPPLER WIND PR
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THE EQUATORIAL ATMOSPHERE RADAR:SYS
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Table 1: Specifications of the EAR
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VHF ATMOSPHERIC AND METEOR RADAR IN
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ased upon a geotechnical engineerin
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VORTICAL MOTIONS OBSERVED WITH THE
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interpolation from the original gri
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A NEW MINIRADAR TO INVESTIGATE URBA
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e eliminated to analyze correctly t
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Session PWG 1: System Calibrations
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Session PWG 2: Data Analysis, Valid
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• the time series vectors x(k) of
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Fig. 4: reflectivity of the hydrome
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Session PWG 3: Accuracies and Requi
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Session PWG 4: International Collab
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Session II.E: NOVEL PERSPECTIVES AN
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2 Proposed AlgorithmReceived signal
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N#4E-1-16E1A1#1#2A-1-1C1#3C-1-19Fig
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of conventional DCMP, with which th
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applying the directional constraint
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while for a beam of finite width, t
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In order to make the process more q
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WHAT IS TURBULENCE SEEN BY VHF RADA
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Enhanced resolution applyingpulse s
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Beckmann, Spizichino, 1964Fig. 8 Po
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Fig. 11 Plots of temporal variation
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Fig. 14 Distributions of phase cent
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Hocking, W.K., Radar studies of sma
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THE STRUCTURE FUNCTION-BASED APPROA
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{ Ui( t), Vi( t), Wi( t)} = { Ui ,
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161). Assumption 2H: the instantane
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Only the second order SF are consid
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fluctuations umk( t ) along the bas
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VHF PARASITIC RADAR INTERFEROMETRYF
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• All the costs of transmitter pr
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Figure 2: Example of range-azimuth
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Target Altitude, km1009080706050403
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ReferencesGriffiths, H. D., A. J. G
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Participants ListAvery, James P.Uni
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Hysell, David L.EAS/Cornell Univers
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Silva, Robert R.ATRADAustraliarsilv
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AAdachi, A. .......................
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TTabary, P. .......................
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