2 . School of Science, Xidian University, Xi’an 710071, China
1 IntroductionHigh frequency (HF) coherent radar backscatter from ionospheric plasma irregularities with a variety of scale lengths from meters to kilometers,also known as radar aurora,is an important high-latitude phenomenon. These irregularities are thought to drift with the bulk plasma motion and are believed to be generated by several kinds of instabilities. Consequently,much emphasis has been givento understanding why and where the se ionospheric irregularities occur,and what the favorable conditions for the ir generation are. In the F region,the irregularities are generated primarily by the gradient drift instability[1, 2] and the current-convective instability[3, 4],whereas in the E regional titude,the bulk of the plasma irregularities are believed to be generated by two possible mechanisms: The modified two-stream instability,also known as the Farley-Buneman instability(FBI),and the gradient-drift instability (GDI),producing two categories of echoes,termed Type I and Type II,respectively. Type I echoes have a low spectral width and a velocity constrained to be near the localion-acoustic speed Cs with a typical value of 350-400 m·s-1at 110 km altitude. Type II echoes have a lower Dopplervelocity and a broader spectral width.
Greenwald et al.[6, 7] developed the concept of the Super Dual Auroral Radar Network (SuperDARN) capable of monitoring extensive regions of both the northern and southern hemisphere polar ionospheres; especially the auroral and polar cap ionospheres. The concept is based on the development of a network of dual radars. Each radar pair comprises two separate radars that have an over lapping field of view,such that the velocity of the irregularities can be determined owing to the different viewing directions of the radars. Currently,SuperDARN consists of more than 30radars globally and the radar data are utilized by scientis ts from all over the world.
In developing the Zhongshan HF radar,the aim hasbeen to extend the SuperDARN coverage in the southe rn hemis pheric,polar cap and auroral regions. Figure 1 shows the fields of view of the SuperDARN radars in the southern hemisphere. The field of view of the Zhongshan radar is depicted as a red fan with a radar bore site of 72.5°. The geomagnetic latitudes of coverage of the Zhongshan radar extend from ~60 MLAT to ~82 MLAT,including the cuspregion,the auroral oval,and the polar cap region. The spatial coverage of Beam 15 includes part of the polar cap region in most MLTs.
A large number of previous observations have concentratedon the characteris tics of ionospheric echoes,eithe r inthe F region[4, 8, 9, 10, 11, 12] or the E region[1, 13, 14, 15, 16],by using VHF,UHF and HF radar. In contrast to UHF and VHF radio waves,high frequency (HF) radio waves are very susceptible to refractive effects. The orthogonality condition can be achieved between the wave vector and the Earth’s magnetic field for the SuperDARN HF radars by the refraction of radio waves in the ionosphere. Hanuise et al. presented the statistical characteris tics of the E region echoes by employing the SHERPA radar at high latitudes. The observed echoes are both Type I and II echoes with the exception of substantially smaller spectral widths. Similarly,both the se two kinds of E region echoes were also found byHaldoupis et al. using a HF radar at mid-latitudes. Different statistical characteris tics of backscatter echoes can be obtained for different SuperDARN radars. Parkinson etal. have analyzed statistically the dis tribution characteristics of echo occurrence,and average Doppler velocity and width in different geomagnetic activities using the TIGERradar data in the Southern Hemisphere. Some studies have also focused on the E region[14, 15, 20] or the F region[9, 11, 21]echoes. Carter and Makarevich presented a statistic alanalysis of E region echoes using the data of TIGER HFradar between November 2004 and December 2006. This revealed two peaks in the morning (03-09 MLT) and eveningsecto rs (15-21 MLT) with the latter peak having a smaller maximum and being prominent only in some monthly periods. A statis tical study of the occurrence of ground and ionospheric backscatter within the fields of view of the CUTLASS HF radars during the first 20 months of operation was undertaken by Milan et al.. They found that the Iceland radar can observe more near-range E region backscatter than the Finland radar owing to the more zonal beam pointing direction. There are also many work[24, 25]with interests in the statistical analysis and initial studies of Super DARN radar echoes,some of which[26, 27] demonstrated the dis tribution difference of backscatter echoes indifferent radar frequency bands.
This paper describes the basic characteris tics of the SuperDARN Zhongshan radar,reporting the diurnal and seasonal variations,the geomagnetic activity and the frequency dependence of ionospheric echoes observed by the Zhongshan radar in its first two years’ operation,during the sunspot ris ing interval from April 2010 to January 2012.2 Zhongshan radar
The Zhongshan high frequency (HF) radar located at Zhongshan Station in Antarctica has been establis hed and in operation since April 2010,supported by the Tenth Five-Year Plan for CHINARE Capacity and the Meridian Space Weather Monito ring Project,whose main objective is to observe polar ionospheric convection. The geographic coordinate of the Zhongshan Station is 69.4°S,76.4°E,the Corrected Geo-Magnetic (CGM) coordinate is 74.5°S,96.01°E,and the invariant magnetic latitude is ~75°S,L =13.9,MLT≈UT+2 h,LT≈UT+5 h. During the condition of quiet geomagnetic and solar activity,Zhongshan Stationis in the cusp region near magnetic noon,in the polar capregion at night,and in and out of auroral oval twice everyday (under the auroral oval during 04-08 UT and 12-15UT). Zhongshan Station has become one of the most important stations for probing and studying the variation of the space environment conditions[28, 29].
Zhongshan HF radar commenced operation as soon as the radar was built and is one of the SuperDARN members.SuperDARN has been establis hed for over 20 years. It began with the Goose Bay radar and has been successful in addressing a wide range of scientific questions concerning processes in the magneto sphere,ionosphere,the rmosphere,and mesosphere,as well as questions relating to general plasma physics[30, 31]. As with the other SuperDARN radars,the spectral analysis of ACFs is made for Zhongshan HFradar echoes backscattered by ionospheric irregularities,and the n the echo power,the line- of -sight Doppler velocity,and the Doppler power spectrum of the irregularities are estimated.
The design of the Zhongshan HF radar is similar to that of othe r SuperDARN radars. It comprises a main array of 16 horizontally polarized log-periodic antennae,each separated by ~15 m,operating in the frequency band from8-20 MHz with both transmit and receive capability,and aninterferometer array of 4 antennae 100 m in front of the main array,which has receive capability only,as shown inFigure 2. It is a stereo HF radar with two radar channels,whose electronics was developed by Leicester University.The Zhongshan HF radar can receive HF backscatter echoes from a slant range of 180 to 3 000 km,and at heights including the ionospheric D region,E region and F region,depending on the number of gates. In common mode,also referred to as normal scan,16 beams are sounded with ad well time of 3 or 7 s,producing field- of -view maps of backscatter echoes with an azimuthal coverage of over 50°,every 1 or 2 min. Each full scan commences on a GPS-synchronized two-minute boundary to ensure that all the SuperDARN radars start the scan simultaneously. Typically,75 range gates are sampled for each beam,with a pulse length of 300 μs,which corresponds to a gate length of 45 km and a lag to the first gate of 1 200 μs (180 km). In this configuration,the maximum range of the radar is approximately3 555 km with each field of view containing1 200 cells. Zhongshan HF radar can work in two channels independently,for example,the all-beams scan mode is operated in channel A,the scan mode of different frequencies,and different range resolutions can be operated in channel B at the same time; thus,data with different spatialand temporal resolutions can be obtained. Zhongshan HF radar can perform different scanning patterns and different range resolutions are possible,which can be changed to study certain areas within various fields of view.3 Stat is tical results
The data used in the statistical calculation were taken between April 2010 and January 2012. All parameters were obtained using the standard SuperDARN FITACF algorithm[32, 33]. To eliminate possible contamination from nonionospheric scatter echoes,those echoes with low velocity(Vlos<30 m·s-1) and narrow width (Δv<35 m·s-1) are identified as ground and sea scatter,which are excluded from the statis tics. The ionospheric dataset is also cleaned by excluding echoes with low power (SNR<3 dB).
Figure 3 summarizes the variations of backscatter occurrence rate with the day of year (DOY) on different beams for the SuperDARN Zhongshan radar. The colored lines are for the 9-day moving average value of the data points for the se four beams. The dis continuities from day117 to day 124 are because of the absence of observation during this period. We found significant differences between the beams. The beam with a larger number can observe more echoes than the beam with smaller numbers.Note that for Beam 15,two maximum occurrence peaks are found near day 92 and day 275 and the occurrence on winter days is obviously larger than that on summer days.There is also a prominent low valley from day 23 to day 26because of strong radio wave absorption arising from a magnetic storm during the se days.3.1 Diurnal variations
Figure 4 shows the diurnal variations of : (a) occurrence rate,(b) average power,(c) average line- of -sight velocity and (d)spectral width of ionospheric echoes for Beams 0,5,10,and 15. The occurrence rate has two peaks at 04-08 UT and16-17 UT,which vary slightly with the different beams.The value of the peak occurrence increases with be am number,and the first peak occurs earlier at smaller number beams,whereas the second peak exhibits the opposite trend.The first peak of occurrence of Beam 0 is ~10% at 04 UT,whereas Beam 15 has the peak near 08 UT with a value of ~18%. The beams with larger numbers can observe more echoes with stronger power than the beams with smaller numbers,as shown in Figures 4a and 4b. For smaller beams,the day side valley of the occurrence is deeper than that of the night side,which is the opposite of that for larger beams.For Beams 0 and 5,the minimum is near 13 UT,and for Beams 10 and 15,the minimum occurs at ~21 UT. Generally,the occurrence and average power have similar behavior and exhibit a double peak structure with the main peak around 04-08 UT and the second peak around 16-17 UT.
In Figure 4c,for the line- of -sight Doppler velocities,the diurnal variation is significantly different among the beams. For Beam 0,the velocities are positive with a maximum of 160 m·s-1 on the day side,which indicates that the motion is to wards the radar,and mainly negative on thenight side with a maximum of -100 m·s-1. The variations of Beam 15 have almost the opposite trend to that of Beam 0;the maximum of the velocities is ~260 m·s-1 around 22 UT for Beam 15.
In Figure 4d,the spectral widths on the day side are of ten higher than those on the night side. At 00 UT,the average widths are 130-140 m·s-1 and increase gradually with UT,peaking around 13 UT,and the n starting to decrease steeply. The minimum appears at ~20 UT. The difference of spectral width among the different beams is not obvious from 00 UT to 11 UT. From 11 UT,the ionospheric echoes observed on Beam 0 have much larger spectral widths than on the othe r three beams. The maximum spectral width on Beam 0 is about 220 m·s-1,whereas it is about 170 m·s-1 for the other beams. This might be because the echoes at near ranges of less than 30 gates on Beam 0 have more opportunities in the cusp region than the othe r beams,as shown inFigure 1b. In the cusp region,the echoes have greater spectral widths around noon,probably as a result of cusp particle precipitations.3.2 Seasonal variations
Figure 5 shows the seasonal variations of : (a) occurrence,(b) average power,(c) average line- of -sight velocity,and (d)average widths of ionospheric echoes for Beams 0,5,10,and 15. The velocities are divided into two parts: positive and negative. For the echo occurrence,shown in Figure 5a,the seasonal variations are more obvious for those beam swith larger numbers with maxim a mainly in September and April. For Beam 15,a prominent maximum occurs in March with a secondary maximum in September,and the echo occurrence in the winter months is of ten larger than that in the summer months. The seasonal variation of average power is similar to that of occurrence,in the way that the average power in winter is larger than that in summer,which might be attributed to a smaller population of irregularities owing to the solar radiation in summer. For the variations of line- of -sight velocities,the values are also obviously larger in the winter months than in the summer months for both the positive and negative components.
In Figure 5d,the seasonal variations of spectral width sare more obvious for those beams with larger numbers. For Beam 15,the spectral widths in the winter months are significantly larger than those in the summer months with a peak value of ~170 m·s-1 and a broader maximum region from April to August. The spectral widths decrease to 120-130 m·s-1 in the summer months from September to February. For Beam 0,the seasonal variations are not obviouswith the value fluctuating between 160 and 180 m·s-1.3.3 Geomagnetic activity dependence
Figure 6 shows the occurrence of ionospheric echoes at different geomagnetic activity levels. (1) For Kp=0 (Figure 6a),the peak occurrence is between the 05-11 MLT and 79°MLAT with a value of ~45%. (2) At Kp<2 (Figures 6a and6b),a region with obviously low occurrence is around22-23 MLT. This is partly due to the greater absorption in this interval associated with auroral subs to rms,and partly due to the polar hole that exis ts in this region at high latitudes[34, 35]. Further more,the electron density of the night side ionosphere is lower than that on the day side and the refractive effect of the ionosphere on radio waves is weak,increasing the likelihood of the HF rays penetrating the ionosphere. (3) When Kp increases to 2 (Figure 6c),the peak occurrence decreases obviously to about 30% between06 and 09 MLT,expanding in MLAT of 76°-79°. When the Kp index increases further to Kp≥3,the peak occurrence is at 23-03 MLT and 76° MLAT. From the geometry of Beam15 of the Zhongshan HF radar,the echoes at lower latitudes correspond to lower gates with lower altitude,and the echo occurrence decreases obviously near 10-14 MLT on the day side. Generally,the peak occurrence on the day side is attributed to echoes at low levels of geomagnetic activity and decreases with the enhancement of geomagnetic activity,whereas it is the opposite on the night side.
Figure 7 shows the average power of ionospheric echoes at different geomagnetic activity levels. From Figure 7,the presence of peak power varies for different values of the Kp index. In quiet times with Kp=0,large values of power are mainly in three regions. The first region is in 76°-79°MLAT from 06-13 MLT with the value greater than 20 dB.The second one is from 14-18 MLT at higher latitude with power of ~16 dB. The third one is at lower latitude 75°MLAT from 19 to 22 MLT. For Kp=1,the region with peak power shifts to 05-15 MLT and 75°-79° MLAT,expanding in MLT and latitude. As the geomagnetic activity increases to Kp=2,the peak power increases from 18 dB with Kp=1to 21 dB with Kp=2.
Figure 8 shows the average line- of -sight Doppler velocities of ionospheric echoes at different geomagnetic activity levels,the tilted dashed lines illustrate the overlay curves of MLT. The velocities increase with the enhancement of geomagnetic activity. For Kp=0 (Figure 8a),the velocitieson the day side have a peak at about 300 m·s-1 and increase to more than 450 m·s-1 at Kp≥3 (Figure 8c). The same feature can also be observed on the night side,which is consistent with the the ory that ionospheric convection is enhanced with increasing geomagnetic activity.
Figure 9 shows the average Doppler spectral widths of ionospheric echoes at different geomagnetic activity levels.As noted in Figure 9,the spectral widths on the day side are larger than those on the night side,which might be related to particle precipitation in the cusp region. The maximum of spectral widths decreases with the increase of geomagnetic activity. The spectral widths are quite low from dusk side tonight side with a value of less than 100 m·s-1,which shifts to higher latitudes when the geomagnetic activity becomes more disturbed. On the night side,the widths tend to be larger at lower latitudes with an increase in geomagnetic activity,which might correspond to the different mechanisms of production of ionospheric echoes. Generally,the Doppler spectral width decreases with increasing geomagnetic activity,which is consistent with the results observed by Fukumo to elal.,using the Syowa SuperDARN radar in Antarctica.3.4 Frequency dependence
The Zhongshan HF radar was in operation with different frequencies in cycle every 2 min in channel B from 3 April to 8 October,in 2010. These frequencies are: 9,10,12,13,14,16,and 17 MHz. The data in the se frequency bands can be used to analyze the echo frequency dependence. Figure 10 shows the frequency dis tribution of echo occupancy rate and average power within this database. As can be observed,the average power is maximum at 9-10 MHz,and decreases slightly with increasing frequency. Regarding the echo occupancy rate,the re are also more echoes observed in lower frequency band.
In summary,for Zhongshan HF radar,the echo counts decrease with frequency. Of the operating frequency bands in 2010,9-10 MHz is the best operating frequency band;however,this might vary under different conditions of solar and geomagnetic activity.
Figure 11 presents the color-coded relative echo countsas a function of range and power for each frequency band with a resolution of 1 gate and 1 dB in power. From Figure 11 we know that the re is a region with obvious ionospheric echoes less than 20 gate and 30 dB,and that the echo counts are more abundant in the low frequency bands.When the operating frequencies are 9 and 10 MHz,the echo power is mainly between 0-30 gate and 0-30 dB in power,and this region becomes narrower in range and power with increasing frequency,which is diminished to be less than 20gate in range and less than 20 dB in power. This might be because radio waves with higher frequency are less susceptible to refractive effects in the ionosphere and tend to penetrate the ionosphere without satisfying the perpendicularity criterion,or it might be due partly to the different character is tics of the irregularities with various scale length observed by radio waves with different frequencies.
Figure 12 shows the ionospheric echo counts as afunction of range and velocity for each frequency band witha resolution of 1 gate (45 km in range) and 25 m·s-1 in velocity.Figure 12 shows: (1) The velocity of most echoes is between -400 m·s-1 and 400 m·s-1; (2) The distribution of ionospheric echoes in range varies for different frequencies.In low frequency bands (9 and 10 MHz),the region with abundant echoes is less than 30 gate and decreases in range with increasing frequency; (3) When the operating frequency increases to 17 MHz,the Doppler velocity is larger from gate 5 to 20. This has to be related to the refractive properties of the ionosphere and its influence on radio wave propagation. Higher frequency waves are refracted less and the trajectories are bent more slowly along the irpropagationpath and must propagate deeper into the ionospheric plasma,and fewer waves are backscattered by ground/sea,such that the contamination by ground scatter echoes is less for higher frequency waves,which accounts for the higher average velocity of echoes.
Figure 13 presents the echo counts as a function of range and spectral width for each frequency. The spectral width of most echoes is less than 300 m·s-1,and with increasing frequency,the width decreases. The echo spectral width is between 0 m·s-1 and 300 m·s-1 for the operating frequency of 9 MHz,while the value is between 0 m·s-1 and200 m·s-1 for the operating frequency of 10 MHz. This is because the ionospheric irregularities that higher frequencies can observe are mainly related to high energy auroral particle precipitation and this kind of spectrum is generally considered to have narrower width.
Figure 14 shows the echo occurrence as a function of beams for different frequencies. The echo occurrence is calculated as follows: First,we calculate the echo countsN(ut) of a beam from gate 0 to gate 74 and the n,the ionospheric echo counts are determined according to the standard SuperDARN s of tware as M(ut); thus,the echo occurrence is M(ut)/N(ut).
As can be seen in Figure 14,the echo occurrence increases with the beam number for operating frequencies less than 13 MHz. For frequencies greater than 13 MHz,the echo occurrence of the center beam has the maximum value.For any frequency band,the minimum occurrence occurson the beam with the lowest number,which might be related to the geographic and geomagnetic location of HF radar beams and the ionospheric convection modes. As the radio waves propagate through the ionosphere,the y are backs cattered by the decameter-scale field-aligned irregularities(FAI) when the Bragg condition is satisfied,i.e.,significant backscatter is generated only if the radar wave vector lies in the plane perpendicular to the structure of FAIs[23, 36]. The orthogonality condition can be achieved between the wave vector and the Earth’s magnetic field forthe SuperDARN radars by the refraction of HF radar waves in the ionosphere.
For the Zhongshan HF radar,the beams with small number (0-5) tend to be aligned with the Earth’s magneticfield direction,which increases the orthogonality difficulty between the radio wave vector and the Earth’s magneticfield; thus,the lower occurrence of echoes.
The region where HF radar can observe the irregularities can be simulated by ray tracing. In the calculation,the orthogonality condition is assumed to be satisfied when the angle between HF radar ray vector and the ambient magnetic field vector is within the range of 90°±1°. In the present study,we introduce IRI-2007 electron density profiles to the ray tracing and the height pr of ile of the plasma frequency,andthe ray tracing plots are shown in Figure 15. There are two distinct regions that signify possible areas in which the radar could observe if irregularities exist. These two regions are the expected locations,in both range and height, of the E region and F region echoes,respectively.
Figure 16 shows the simulation results for 10 and 16MHz. As can be seen,in the low frequency band (10 MHz),the beams with larger number can observe the irregularities in a larger region and a greater number of irregularities can be observed. When the frequency is increased to 16 MHz,the beams near the center can observe more irregularities,which is consistent with the observations from Figure 14.4 Dis cussion
Many previous works have reported on the statis tical study of the characteris tics of SuperDARN backscatter echoes,some of which have concentrated on the diurnal,seasonal,and geomagnetic activity variations of backscatter,and the physics of the mechanisms involved has been dis cussed.
Using the SuperDARN Syowa east radar data in 1995,Fukumoto et al. analyzed the effect of geomagnetic activity on echo power,line- of -sight velocity and spectral widths,and summarized that the average echo power and Doppler velocity increase,and the spectral widths decrease with the enhancement of geomagnetic activity. This is consistent with the results in this study. Ruohoniemi and Greenwald presented statistical results using the GooseBay HF radar and showed that the re is significant dependence on Kp and season for echo occurrence; the highe strates of occurrence were obtained on the night side for quiet conditions and in the afternoon for dis turbed conditions and winter was the most active season. Some of the ir results are similar to our results,whereas others are different from those obtained in this study owing to the different location sand beam pointing of the radars. In this study,the data are mainly polar cap echoes from 2010 to 2012,which was a time of increasing solar activity and the backscatter is mainly from auroral oval and the poleward edge of the auroral oval. Carter and Makarevich presented the E region diurnal variations and the effect of geomagnetic activity.It is found that the E region echo occurrence for individual radars exhibits very similar diurnal variations forlow geomagnetic activity,but that the differences between radars increases with increasing activity. Ballato re et al.considered the rate of scattering occurrence over a two-year period from six SuperDARN radars operating in the Northern Hemisphere and found that the HF scattering occurrencedepends on the MLT,the magnetic latitude,and the local season,which was in agreement with previous observations[39, 42]. Their results could be interpreted in terms of the sunlit suppression of ionospheric density gradients bymore intense summer photo ionization.
The statis tical results in this paper demonstrate that for the echo occurrence of the SuperDARN Zhongshan radar the re are two minima,which are near 13 UT and 21 UT. For Beam 0,the minimum is at 13 UT and a secondary minimum is at 21 UT,while for Beam 15,the minimum is at 21UT and a secondary minimum is at 13 UT. The higher occurrence of echoes can be observed on Beam 15 than on Beam 0. Considering the beam pointing of Beam 0 and 15,Beam 0 is closer to the auroral oval than Beam 15. The two minimums of occurrence arise from the enhanced D region absorption associated with is olation and particle precipitation that attenuate the propagation of HF radio waves,especially under the auroral oval near 13 UT,and the absorption event associated with sub storms that are frequent at 21UT. For Beam 15,the absorption from subs to rms and the little signal received from backscatter owing to the existence of the polar hole might be more prominent at 21 UTthan the absorption from the D region at 13 UT,leading to the minimum near 21 UT.
Regarding the effect of geomagnetic activity on echo occurrence of Beam 15 in the grid of MLT and MLAT,the echo occurrence is at different latitudes at different values of the Kp index. At quiet times (Kp<2,Figures 6a and 6b),agreater number of echoes can be observed near 80° MLATon the day side. With an increase of geomagnetic activity to the value of Kp≥3,a greater number of echoes are observed near 76° MLAT on the night side. Generally,ionospheric echoes received at ranges of less than 900 km quite of ten originate from the E region,and sometimes from both the E and F regions,and this is slightly different for different radars. After considering the pointing direction of Beam 15,it is known that the echoes at the se two latitude regions might come from different heights in ionosphere. Atquiet times (Figures 6a and 6b),the echoes at higher latitudes might come from higher parts of the E region or Fregion,and at dis turbed times (Figure 6d),the echoes at lower latitudes might be from lower parts of the E region.This is because particle precipitation during high geomagnetic activity leads to a large electron density in the lower ionosphere and thus,more irregularities are formed. Furthermore,the absence of the D region on the night side ionosphere leads to little absorption of radio waves and thus,a greater number of echoes are observed at lower latitudes(lower ionosphere). This is in agreement with the findingthat higher spectral widths can be observed at lower latitudes on the night side for higher geomagnetic activity,asshown in Figure 9d.
The diurnal variations of line- of -sight velocities are very obvious. For Beam 0,the velocity is mainly positiveon the day side and negative on the night side,which is the opposite of the variations for Beam 15. This is consis tentwith the fact that ionospheric convection is mainly antis unward in the polar cap region and sunward in low latitudes.The variations can be explained from Figure 17.
At 11 UT (Figure 17b) Beam 15 is mainly pointing to the night side and the negative velocity (away from the radar) is consistent with the anti-sun ward flow in the polar capregion,and the positive velocity on Beam 0 is consistent with the sun ward flow in low latitudes. This is related to the wide azimuthal coverage of SuperDARN with values of greater than 50°. At 23 UT,shown in Figure 17d,Beam 15is mainly pointing to the day side and the positive velocity(to wards the radar) is also consistent with the anti-sunward flow in the polar cap region,and the negative velocity on Beam 0 is also consistent with the sun ward flow in low latitudes. The increase in velocities with the enhancement of geomagnetic activity is in agreement with the the ory that ionospheric convection is enhanced with increasing geomagnetic activity. The velocity variations at othe r times are also the result of projections of the west and east components of ionospheric convection on the beam pointing direction,as shown inFigure 17a and 17c.
The spectral widths are thought to be enhanced by large-scale velocity gradients,convection turbulence,and Pc1-2 hydromagnetic wave activity. Generally speaking,the spectral widths are larger in the region of open magnetic field lines on the day side,which is also confirmed in this study. In addition,the statistics in this study also confirm that the spectral widths decrease with the enhancement of geomagnetic activity,because more high energy particles are precipitated at high geomagnetic levels,and because spectral widths from high energy particles are relatively lower than those from low energy particles. This is also consistent with the results of Fukumo to et al..
We have found a marked seasonal effect on the backscatter echoes. The occurrence rate,average power,average line- of -sight velocity,and spectral widths are lower in summer than in winter. This might be related to the more intense photo ionization in summer,which leads to the suppression of density gradients. This is consis tent with the results of previous studies.5 ConclusionsIn this study,we present the statis tical characteris tics of ionospheric echoes based on the first two years’ observations of the Zhongshan radar. These include diurnal variations,seasonal variations,geomagnetic activity,and frequency dependence. The main results are summarized asfollows:
(1) Double peak structures can be observed for the diurnal variations of occurrence rate and average power,which are at 04-08 UT and 16-17 UT with a slight difference between the beams. The line- of -sight velocities for Beam 0 are mainly positive on the day side and negative on the night side,which is the opposite trend to that of Beam15. These variations correspond to the anti-sunward flow in the polar cap region and the sun ward flow in lower latitudes of the ionospheric convection map. The spectral widths on the day side are of ten higher than those on the night side,which is related to particle precipitation in the cusp region and Beam 0 has the most prominent peak with a value of 220 m·s-1 around 13 UT.
(2) The seasonal variations are more obvious for the beams with larger numbers. The occurrence,the average power,the line- of -sight velocity,and the spectral widths are generally larger in the winter months than those in the summer months.
(3) The difference is significant for different geomagnetic activity levels for Beam 15. Generally,the occurrence rate decreases with geomagnetic activity on the day side and increases with it on the night side; this arises from the solar radiation and absorption difference in MLT under the conditions of different geomagnetic activity levels. The line of -sight velocities increase with increasing Kp,while the Doppler spectral widths decrease with increasing geomagnetic activity.
(4) Of the frequency bands from 9 to 17 MHz used in2010,9-10 MHz is the best operating frequency band,but this might vary under different conditions of solar and geomagnetic activity.
(5) The difference of occurrence between beams is related to the beam pointing direction,and the different regions that the radar can observe for different frequency radio waves,arises from the area in which the orthogonality condition between the wave vector and the Earth’s magnetic field is achieved.
The Zhongshan HF radar is an important component of SuperDARN,extending the coverage of the network in the polar cap region and the auroral regions in Antarctica.Further new dis coveries can be expected in the future.Acknowledgments This work was supported by the National Natural Science Foundation of China (Grant no. 41031064),the Ocean Public Welfare Scientific Research Project of China (Grant no. 201005017) and the Chinese Meridian Project,the Chinese Polar Environment Comprehensive Investigation & Assessment Programmes (Grant no. CHINARE 2012-02-03). Data were is sued by the Data-sharing Platform of Polar Science (http://www.chinare.org.cn) maintained by Polar Research Institute of Chinaand Chinese National Antarcic &Arcic Data Center.
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