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on the decoded raw data profiles to decrease further the peak to side-lobe levels (from -22 dBto less than -32 dB) at the expense of spreading the side-lobe contamination into moreranges. This second filter is needed in order improve the discrimination between head andtrail echoes.Once the Doppler velocity for optimum decoding is found, the raw voltages for eachof the channels are decoded and signal statistics are recorded. Then we proceed by findingthe range where the power is highest for each profile. Working with the ``peak'' signalstatistics is much faster, allowing us to test and implement robust algorithms for meteorcharacterization. We have been able to measure directly, the initial range, the range coverage,signal-to-noise ratio, radial velocities (using three methods), and duration of the meteor,radial decelerations, and azimuth of meteor trajectory. In addition, we are able to derive theabsolute velocities and decelerations, and elevation angles.3. ResultsOur observations have been mainly conducted around Leonid meteor showers since1998. However we have recently started observations at different seasons. Statistically, weare observing similar characteristics during Leonid and non-Leonid events in velocity,deceleration and altitude distributions. In Figure 3, we show examples of where meteors arecoming from during a Leonid (left) and non-Leonid (right) event. The sky maps show theprojected Ecliptic plane (solid black curve), some constellations for reference, and theEarth’s Apex (thick star) for the given time. Each meteor observed around 0700 LT arerepresented with circles. The absolute velocity is color-coded and the size is proportional tothe signal-to-noise ratio (SNR).1364. Summary and ConclusionsAs it has been shown in previous sections, we have successfully implemented atechnique to observe and characterize meteor head echoes at equatorial latitudes. The use ofthe large power-aperture capabilities at Jicamarca has allowed us to observe a high rate ofmeteors (more than 3000 per hour) in the small volume subtended by the 1 o antenna-beam.Moreover, using interferometry, we have been able to characterize the three-dimensionalcomponents of meteor velocities in the Earth's frame of reference.Our results do not show any evidence of the Leonid meteor showers, in agreement toresult reported by other large power-aperture radars. We have shown that meteor parametersduring both Leonid and non-Leonid events are statistically similar (range of occurrence,velocity distribution, deceleration distribution, origin). Apparently, we detect only the verysmall sporadic meteors, which are much more abundant than the larger meteors associated tomajor meteor showers and which seldom cross the 1 o antenna beam.Besides providing meteor-head observations at a unique frequency (50 MHz) andlocation (equatorial latitudes), our results are particularly important for the 3Dcharacterization of meteor heads. We have shown, at different seasons that the velocitydistribution of meteors respect to the Earth's frame of reference is clustered around the EarthApex, within ±18 o transverse to the Ecliptic and narrow (±8.5 o ) in heliocentric longitude inthe Ecliptic plane. A change to a solar inertial frame of reference, roughly double the widthsof these distributions, since most of the meteors have a relative velocity which is about twicethe orbital velocity of the Earth. The velocity representation in heliocentric coordinatesincluding the gravitational attraction as well as its orbital distribution will be left for a futureeffort.So far, our observations have been concentrated around sunrise time when the EEJare expected to be weak. In the future, we plan to extend our observations to other times,
particularly during daytime counter electrojet conditions when EEJ are also expected to beweak. Moreover, we plan to continue improving the technique in order to get better timecoverage as well as more precise parameters.More results are presented and discussed in detail by Chau and Woodman [2003].AcknowledgementsThe Jicamarca Radio Observatory is operated by the Instituto Geofísico del Perú, withsupport from the NSF Cooperative Agreement ATM-9911209 through Cornell University.Figure 3. Sky maps representing where meteors are coming from for a Leonid (left) and non-Leonid (right)events, around 0700 LT. Each meteor is represented with circles, the absolute velocity is color-coded and thesize is proportional to SNR.BibliographyChau, J. L. and R. F. Woodman, Observations of meteor-head echoes using the JicamarcaVHF radar in interferometer mode, Atmos. Chem. Phys., submitted, 2003.Chapin, E. and E. Kudeki, Radar interferometric imaging studies of long-duration meteorechoes observed at Jicamarca, J. Geophys. Res., 99, 8937-8949, 1994.Close, S., S. M. Hunt, F. M. McKeen, and M. J. Minardi, Characterization of Leonid meteorhead echo data collected using the VHF-UHF advanced research rpjects agency longrangetracking and instrumentation radar (ALTAIR), Radio Sci., 37,10.1029/2000RS002602, 2002.Dyrud, L. P., M. Oppeneheim, S. Close, and S. Hunt, Interpretation of non-specular radarmeteor trails, Geophys. Res. Lett., 10.1029/2002GL015 953, 2002.Elford, W. G., Novel applications of MST radars in meteor studies, J. Atmos. Sol. Terr.Phys., 63, 143–153, 2001.Farley, D. T., Theory of equatorial electrojet plasma waves: New developments and currentstatus, J. Atmos. Sol. Terr. Phys., 729–744, 1985.Janches, D., M. C. Nolan, D. D. Meisel, J. D. Mathews, Q. H. Zhou, and D. E. Moser, On thegeocentric micrometeor velocity distribution, J. Geophys. Res., 108,10.1029/2002JA009789, 2003.Sato, T., T. Nakamura, and K. Nishimura, Orbit determination of meteors using the MUradar, IEICE Trans. Commun., E83-B, 1990–1995, 2000.Woodman, R. F. Inclination of the geomagnetic field measured by an incoherent scattertechnique, J. Geophys. Res., 76, 178-184, 1971.137
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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
Page 92 and 93: THE ROLE OF UNSTABLE SPORADIC-E LAY
Page 94 and 95: (σ H / σ P )E y (where σ H and
Page 96: STUDY OF A LOW E-REGION QUASI-PERIO
Page 99 and 100: 100 m/syrFigure 4: Geometry of the
Page 101 and 102: Where the notations carry same mean
Page 103 and 104: Where dx/dt and dy/dt are the veloc
Page 105 and 106: non-negativity of the image is prio
Page 107 and 108: spectrum corresponding to the backs
Page 109 and 110: The Artigas and Machu-Picchu Statio
Page 111 and 112: Arguments against the second altern
Page 113 and 114: Extension of the Kolmogorov spectru
Page 115 and 116: volumeESRvolumeSSRSSR SSRESR ESRSSR
Page 117 and 118: individual particles in a statistic
Page 119 and 120: Anomalous spectraTalkner [4] studie
Page 121 and 122: To observe the E region FAI echoes,
Page 123 and 124: matter daytime or nighttime and are
Page 125 and 126: two sub-arrays, each sub-array made
Page 127 and 128: 4. SummaryHere we describe a radio
Page 129 and 130: Figure 1. E-region DPS4 spectra, ri
Page 131 and 132: effects. It is therefore plausible
Page 133 and 134: 1996 and high in 2002). The electri
Page 135 and 136: electric fields map along the geoma
Page 137 and 138: SNR condition is always difficult a
Page 139 and 140: Figure-4 Power spectrum plots of a
Page 141: As we show below, Jicamarca offers
Page 145 and 146: where ˆδ nm = (δ l − δ m )
Page 147 and 148: PMSE is more easily interpreted as
Page 149 and 150: ResultsTemperature climatology• s
Page 151 and 152: Simultaneous PMSE and NLC observati
Page 153 and 154: ResultsSeasonal variationMSE are no
Page 155 and 156: Figure 2: MSE parameters as functio
Page 157 and 158: Session I.3: Winds, waves and turbu
Page 159 and 160: poor. It was shown that poor perfor
Page 161 and 162: The use of diffraction pattern simi
Page 163 and 164: F 13 (ξ x ′) = (1 − cos 2ψ N)
Page 165 and 166: Figure 3: (a) Baseline length depen
Page 167 and 168: 3. ResultsFigure 1 shows the amplit
Page 169 and 170: variability.Figure 4 shows the aver
Page 171 and 172: Figure 1. Period-time amplitude wav
Page 173 and 174: the 12-h and 24-h periodicities in
Page 175 and 176: winds and variances at altitudes 70
Page 177 and 178: similar correlation with larger mag
Page 179 and 180: of the refraction index are not equ
Page 181 and 182: Fig. 8. Zonal wind (top) and temper
Page 183 and 184: STUDIES ON ATMOSPHERIC GRAVITY WAVE
Page 185 and 186: 1100-1200 hours. From this plot 6.3
Page 187 and 188: STUDIES ON WINDS AND MOMENTUM FLUXE
Page 189 and 190: 3.4 Monthly variation of momentum f
Page 191 and 192: 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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presented in Praskovsky et al. (200
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In Fig. 2 a sketch of a mountain le
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In Fig. 8 the lamina is aligned on
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Figure 1: composite day (13 days) o
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virtual sensible heat fluxes ( Wm-2
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3. Characteristics of precipitation
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Fig. 3: Horizontal distribution of
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3. Results and discussionUHF profil
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Figure 4. Monthly variation of slop
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system with two receiving antennae,
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cycle of precipitation. Figure 3(a)
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Histogram of Zonal Velocityh=5.13 K
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5. Summary of results and concludin
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the two nearby major cities, Chenna
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Boundary layer height, km32.521.5(a
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Figure 1:Data from the MST radar at
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spectral processing. In this partic
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3. Results and discussionIn the pre
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4. SummaryAn attempt has been made
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The purpose of this study is to exa
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Figure1. Three-day average of momen
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3. The improved method to estimate
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But in case of period until 1800 UT
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Session I.5: Operational Aspects an
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The profilers of WINDAS weredesigne
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NOAA, 1994 : Wind profiler assessme
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FIRST RESULTS OF THE BOUNDARY LAYER
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Figure 3. Pulse Design Diagram to s
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MOVEABLE UHF/S-BAND PROFILER/DISDRO
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one-minute Z values determined from
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TOWARD A MULTISENSOR GROUND BASED R
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3. Cloud Evolution Case StudyOn the
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DEVELOPMENT OF A DIGITAL RECEIVER F
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Experiment 1 Experiment 2IPP 999Km
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ELECTRONIC DIGITAL BEAMFORMING IMPL
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The main element of the unit (figur
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.ON-LINE ADAPTIVE DC-GROUND-CLUTTER
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esulting in a widening of the bandw
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ON THE RADIATION EFFICIENCY OF COCO
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Table 2: Experiment #1 results, Tra
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A NEW NARROW BEAM MF RADAR AT 3 MHZ
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Off-zenith beams towards N, S, E, W
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95ALWIN VHF radar: signal powerdB80
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ANTENNA BEAM VERIFICATION USING COS
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Figure 2: A 45 MHz reference sky te
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AN ATTEMPT TO CALIBRATE THE UHF STR
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is at 4.7 km, but in the first 4-ga
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QUALITY CONTROL FOR DOPPLER WIND PR
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The resulting moments are subjected
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SOUSY RADAR AT JICAMARCA: SYSTEM DE
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NEControl andcomputer roomCompCoute
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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
Page 421 and 422:
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
Page 459 and 460:
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
Page 465 and 466:
Hocking, W.K., Radar studies of sma
Page 467 and 468:
THE STRUCTURE FUNCTION-BASED APPROA
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{ Ui( t), Vi( t), Wi( t)} = { Ui ,
Page 471 and 472:
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
Page 477 and 478:
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
Page 485 and 486:
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
Page 491 and 492:
Silva, Robert R.ATRADAustraliarsilv
Page 493 and 494:
AAdachi, A. .......................
Page 495:
TTabary, P. .......................
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