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Aspect angle sensitivity of pump-induced optical emissions at EISCAT
Earth, Planets and Space volume 66, Article number: 159 (2014)
We investigate the aspect angle sensitivity of the pump-induced artificial optical emissions in the ionosphere over the European Incoherent Scatter Scientific Association (EISCAT) high-frequency transmitter facility at Ramfjord, Norway, as a function of the pump beam launch angle relative to the magnetic field line direction. The highest intensity optical emissions occur when the pump beam pointing direction is in the magnetic zenith (approximately 12° S of local zenith). For pump beam directions further north from field aligned, the optical emission intensity decreases for the same pump power. In addition, the primary photon-emitting region becomes displaced towards the magnetic zenith relative to the pump beam and for larger aspect angles, the brightest emissions were found to be outside the −3-dB pump beam width. The Cooperative UK Twin-Located Auroral Sounding System (CUTLASS) coherent scatter high-frequency (HF) radar detected a quasi-constant level of backscatter power from the pumped ionosphere, indicating that saturated striations were formed for all pump beam directions. This indicates that the presence of upper-hybrid resonance is not sufficient to explain the angular sensitivity of the optical emissions.
The production of artificial optical emissions by high-power, high-frequency (HF) radio waves has been observed at high-latitude locations such as the European Incoherent Scatter Scientific Association (EISCAT) facility (Rietveld et al. ) since 1999 (Brändström et al. ; Kosch et al. ) and prior to this at lower-latitude facilities such as Platteville (Haslett and Megill ) and Arecibo (Bernhardt et al. ). The HF electromagnetic wave causes plasma wave instabilities (e.g. Langmuir turbulence and upper-hybrid (UH) waves) to grow close to the pump wave reflection height where the plasma frequency (f p ) equals the pump frequency (f o ). These electrostatic waves can be stimulated by the parametric decay instability (PDI), thermal parametric instability (TPI) or upper-hybrid resonance (UHR) (Kosch et al. [2007a]). The plasma waves not only heat the bulk plasma but also efficiently accelerate ambient electrons to suprathermal energies great enough to excite atomic oxygen. Upon decaying to their ground state, a photon is emitted. The most commonly observed states are the O(1D) (red-line at 630 nm) and O(1S) (green-line at 557.5 nm) with excitation thresholds of 1.96 and 4.17 eV (Gustavsson et al. ), respectively. Due to the lower excitation threshold of the O(1D) state and greater collision cross-section, the intensity of this emission is greater than the O(1S) state by a factor of approximately 4 to 6 (Gustavsson et al. ). Modelling of the electron temperature enhancements in the interaction region accounts for only one-third of the total O(1D) emission intensity. This points towards a modification of the Maxwellian electron energy spectrum whereby strong acceleration causes a higher flux of suprathermal electrons (Gustavsson et al. ). Observations of N2+(1 NG, blue-line, 427.8 nm) (Holma et al. ), with an excitation threshold of 18.6 eV, confirm this.
The primary mechanism thought to accelerate electrons to suprathermal energies is believed to be UHR (Kosch et al. [2002a]). This occurs in the altitude region where the pump frequency is close to the UH frequency (fUH):
where f c is the electron gyro-frequency. At this altitude, which is typically 200 to 250 km for f o = 4 to 8 MHz in the ionosphere over EISCAT, the pump wave couples to UH waves which efficiently heat the plasma (Robinson ). Striations, which are small-scale (1 to 10 m) field-aligned electron density depletions of a few percent (Kelley et al. ) and tens of kilometres long (Senior et al. ), form parallel to the magnetic field due to the TPI (Grach et al., ; Robinson ). Very low pump powers are required to create and maintain striations (Wright et al. ). To stimulate optical emissions, a pump power threshold must be exceeded and this corresponds to the threshold for UHR (Bryers et al. ). We note that pump-induced striations and naturally occurring field-aligned irregularities are entirely equivalent.
Pump-induced striations are much weaker when the pump frequency is close to a multiple of the electron gyro-frequency at the UHR height (Ponomarenko et al., ) because in this regime, UH waves are forbidden (Grach et al., ). The simultaneous growth/decay of striations and O(1D) optical emissions were observed where the pump frequency was varied in small increments about the third gyro-harmonic (Kosch et al. [2002a]), indicating that UHR is important for electron acceleration to suprathermal energies. The downshifted maximum (DM) feature of stimulated electromagnetic emission (SEE) spectra is associated with striations (Leyser, ). The DM minimises when pumping close to the gyro-harmonic (Sergeev et al., ; Stubbe et al. ). Robinson et al. () showed that bulk plasma temperature enhancements and anomalous absorption were minimised when pumping on an electron gyro-harmonic. Collectively, all these observations show the vital importance of UH waves for plasma heating and suprathermal electron acceleration.
Early experiments performed at the EISCAT HF transmitter facility (Kosch et al. , [2002b]) and High Frequency Active Auroral Research Program (HAARP) (Pedersen and Carlson , Pedersen et al. ) showed the unexpected result that the pump-induced optical emissions were most intense close to the magnetic zenith (approximately 12° S of zenith at EISCAT). When the pump beam was directed between vertical and the magnetic field direction, the brightest optical emissions appeared displaced towards the magnetic zenith at EISCAT (Kosch et al. ; Rietveld et al., , ), HAARP (Pedersen and Carlson , Pedersen et al. ,  and Sura facilities (Grach et al., , ). This included cases where the most intense optical emissions occurred outside of the −3-dB locus of the pump beam for pumping in the vertical direction. Pedersen et al. () determined an optical efficiency for O(1D) of 4 R/MW of effective radiated power (ERP) pump power in the magnetic zenith (15° from zenith at HAARP), 1.5-R/MW ERP in the vertical and 0.5 R/MW for aspect angles greater than 15° to 20°.
Mechanisms have been proposed to explain the increased optical emission intensities in the magnetic zenith. Gurevich et al. () showed that the HF pump wave can self-focus on bunches of striations and be ducted to higher altitude in the magnetic zenith. Kosch et al. ([2007b]) showed that the pump beam forms a large-scale density depletion generating a reflective concave HF mirror which focuses the pump wave energy into a small region when pumping in the magnetic zenith. However, our understanding remains incomplete.
The EISCAT UHF 930 MHz incoherent scatter radar (Rishbeth and van Eyken ) was used to observe the aspect angle sensitivity of pump-induced electron temperature enhancements. Rietveld et al. (, ) found that bulk electron temperature enhancements maximised along the magnetic field line direction (approximately 2,800, 1,400 and 1,100 K for 12°, 6° and 0° S). When pumping in the vertical direction, the reduced electron temperature enhancement was displaced towards the magnetic zenith. Unfortunately, cloud eliminated most of the optical observations during this experiment; however, O(1D) photon production was observed to maximise in the magnetic zenith (approximately 12° S) when the pump beam was directed 6° S of vertical.
The results presented above show that both pump-enhanced thermal (as observed by incoherent scatter radar) and suprathermal (as observed optically) electrons have significant aspect angle sensitivity, with maximum response usually in the magnetic field-aligned direction. Pedersen et al. (, ) used a range of pump frequencies (2.83, 2.84, 3.3, 4.3, 4.8, 5.8 and 7.8 MHz) at HAARP. We report on the optical observations from an EISCAT experiment using a different pump frequency (4.04 MHz) as well as observations by HF coherent backscatter radar observations of the UHR. We also include D-region HF absorption into our optical efficiency calculation.
Methods and experiment
The experiment was carried out between 15:40 to 17:50 UT on 3 November 2000 at the EISCAT ionospheric modification facility (Rietveld et al. ), near Tromsø, northern Norway (69.58° N, 19.21° E). The pump frequency was 4.04 MHz with 120-MW ERP with a −3-dB beam width of approximately 15°. The pump wave polarisation was O-mode and operated in a 2-min cycle. For 15:40 to 17:00 UT, the beam-pointing direction is varying between −12°, −6°, vertical, +6° and +12° north with no pump-off periods. From 17:04 to 17:50 UT, the pump cycle changed to 2 min on and 2 min off with the following sequence of beam-pointing directions: −12°, −12°, −12°, −12°, −6°, −6°, −6°, −12°, −12°, −12°, −12° north.
During this period, the EISCAT incoherent scatter radars were undergoing maintenance and consequently were not in operation. A colocated Digisonde recorded ionograms every 12 min. The local plasma density profile was obtained by standard ionogram analysis, i.e. using the fixed relationship between plasma frequency and electron density plus converting virtual range into real height by adjusting the time-of-flight for refractive index. This was used to determine whether the ionosphere was over or under dense at 4.04 MHz. Plasma resonances occur only when the pump frequency is below or slightly above the critical frequency (e.g. Kosch et al. [2007a]).
During the experiment, the digital all-sky imager (DASI) (Kosch et al. ) observed the optical emissions created above the EISCAT facility. The DASI system was located at Skibotn (69.35° N, 20.36° E), approximately 51.5 km (44.1 km east and 26.5 km south) from EISCAT. The imager was pointing into the local zenith with a field of view of 50°. Narrow-band optical filters at 630-nm (O1D, 15:40 to 17:00 UT) and 557.7-nm filters (O1S, 17:00 to 17:50 UT) were used with 10-s integration time. The camera location and orientation was calibrated using the known locations of the stars in the sky for any time. The lens third-order angular transfer function was also computed by fitting the star positions. From these outcomes, the EISCAT pump beam was mapped onto the image for any beam pointing direction and altitude. Ray tracing through the ionosphere was used to determine the HF beam refraction, which resulted in some deviation from the straight line of sight. The last image from a pump-off period was used for background subtraction of all subsequent images of the following pump-on period. Where there was no pump-off period, the image for the +12° north position served as the background image for all other pump beam pointing directions. The changing background image was necessary to compensate for the effect of changing twilight after sunset. Both background and data images were filtered using a 3 × 3 median filter to reduce pixel noise. Both optical wavelengths (557.7 and 630.0 nm) were calibrated in absolute Rayleighs (1 R = 1010 ph.m−2.s−1) using a standard radioactive fluorescent source. The same source was used to determine the lens transmission loss as a function of viewing angle.
The Cooperative UK Twin-Located Auroral Sounding System (CUTLASS) HF radar at Hankasalmi, Finland (62.32° N, 26.61° E), is part of the SuperDARN network (Greenwald et al. ; Chisham et al. ). The radar measures the coherent backscattered power from the pump-induced field-aligned striations. Beam number 5 points over EISCAT through the heated region, with the first range sample (gate) set at 480-km distance, a range resolution of 15-km and a temporal resolution of 1 s. In this configuration, range gate 32 is typically over EISCAT depending on altitude and ray refraction (Senior et al., ). High levels of backscatter indicate the presence of striations (magnetic field-aligned plasma irregularities) and are a proxy for the presence of UH electrostatic waves (Kosch et al., [2002a]). The Bragg backscatter condition, upon which the coherent radar relies, requires the k-vector of the radar and to be perpendicular to the striations, i.e. orthogonality at backscatter must apply.
Results and discussion
Figure 1 shows a keogram for the O(1D) 630-nm emissions without background subtraction between 15:40 and 17:00 UT. The keogram is produced by taking a slice through each image in the north–south plane where the emission centre is located. The y-axis relates to the zenith angle of the pump beam as viewed from the camera location. The horizontal displacement between EISCAT and Skibotn and the pump wave reflection altitude (approximately 280 km) have been taken into account. The black bars show the direction of the pump beam which was varying between −12° and +12° N. The decaying background intensity is due to the setting sun. At around 16:15 UT, the sun appears to have set fully in the ionosphere and the background intensity remains relatively constant.
The most intense optical emissions were found for the −12° and −6° N beam-pointing directions. For other positions, the optical emission intensity decreased significantly. For the −12° N beam direction, there is a tendency for the emitting region to be displaced slightly towards the vertical position. For the other beam directions, the most intense emitting region is clearly displaced towards the field-aligned direction (12° S) with a reduced emission within the beam centre. At 16:10 UT, the optical emissions cease even for the −12° and −6° N beam positions. However, it appears that the emissions in the northward directions remain. This is investigated below.
Figure 2 shows a keogram plotted for the O(1S) 557.7-nm emissions without background subtraction between 17:04 and 17:48 UT. Again, the horizontal displacement between EISCAT and Skibotn and the pump wave reflection altitude (approximately 260 km) have been taken into account. The black bars show the direction of the pump beam which was varying between −12° and −6° N. Here again, it was observed that the maximum pump-induced optical intensity occurs between −12° and −6° N. Enhanced optical emissions at angles greater than −6° N are due to natural particle precipitation.
The top panel in Figure 3 shows the CUTLASS backscatter data from beam 5 over EISCAT. The bottom panel shows the CUTLASS radar (blue), pump (red) and ionospheric critical (foF2, black) frequencies. Range gate 32 is approximately over EISCAT. The CUTLASS radar was controlled manually in order to find the correct frequency to optimise backscatter from the heated region. By varying the frequency of the radar, the propagation path changes since refraction is frequency dependent. Up until approximately 16:25 UT, the radar frequency was changing and it is not clear whether the backscatter is natural or pump-induced in nature. From approximately 16:25 UT onwards, the backscatter is uniform and well structured for range gates 27 to 40, each of 15 km, indicating that it is from the pump-induced striations.
Between approximately 16:00 and 16:35 UT, the Digisonde data shows that the ionosphere was slightly under-dense to the pump wave. However, the pump wave can still stimulate UHR in this situation. This is clearly true for times after approximately 16:25 UT. The under-dense ionosphere could explain why around 16:10 to 16:20 UT, no striations are detected by CUTLASS. However, the orthogonality condition for backscatter may also not have been satisfied. Figure 1 shows that the optical emissions reduce significantly even at the −12° N position around approximately 16:10 UT. This indicates that UHR was not occurring at this time and that the ionosphere was in fact under-dense at 4.04 MHz. The onset of optical emissions at approximately 16:20 UT agrees with the detection of backscatter again in Figure 3 at the same time. The extended period where the pump frequency is less than the critical frequency up to 16:35 UT could be because the Digisonde samples from a wide region in space and the ionosphere is not smooth so there are regions which are under-dense and over-dense within the field of view.
After 17:00 UT when the pump cycle changes to 2 min on, 2 min off, there also appears to be a gap of reduced or nonexistent backscatter close to the 32nd range gate. Possible explanations are that the ionosphere is under-dense in this region of space or that the CUTLASS radar orthogonality condition for backscatter breaks down here so no signal is received.
The region above EISCAT where backscatter is found covers 13 range gates of 15 km, i.e. 195 km in width, since the HF radar ray intersects the heated region approximately horizontally. The heater −3-dB beam width is approximately 15°. When pointing vertically, this gives a region of 71 km across at 270 km in altitude (as indicated by the mean Digisonde data). This indicates that even outside the −3-dB beam width, the power of the pump wave is high enough to stimulate UHR. This is consistent with Wright et al. () who showed that less than 4-MW ERP was required to create and maintain striations. Hence, one might expect that electrons could be accelerated to high enough energy needed to create optical emissions for a large range of zenith angles.
The red line in the top panel of Figure 4 shows the background subtracted intensity for the O(1D) 630-nm emission centred on the magnetic zenith. Since there were no periods where the pump beam was off, the image for +12° N beam position was used as the background. Here, optical emission enhancements were weakest or nonexistent. The black line shows the optical emission intensity centred on the beam-pointing direction. When pumping at −12° N, the same data is shown. The arrows make clear the −12° N pointing direction. As the pump beam aspect angle increases, the optical emission intensities generally decrease. The only exception is sometimes in the magnetic zenith for pump beam direction of −6° N where the optical intensity may remain quasi-constant (e.g. pump cycle at 16:20, 16:40 and 16:50 UT) or even increase (e.g. pump cycle at 15:40 UT). The magnetic zenith (12° S) generally has the higher optical intensity even though more pump power is available to accelerate the electrons in the beam-pointing direction. For northward pump beam directions, the optical emission intensity falls close to zero. The negative values are due to using +12° N images for the background subtraction where clearly the emission intensity was not zero. The error is limited to less than 10 R.
The green line in the top panel of Figure 4 shows the background subtracted pixel intensity centred on the magnetic zenith for the O(1S) 557.7-nm emission. When the pump beam points in the −6° N direction, the emission intensity is very similar (see Figure 2) and therefore is not shown.
The bottom panel of Figure 4 shows the CUTLASS radar data averaged over range gates 27 to 40. As pointed out above, the backscatter from 15:40 to 16:20 UT is difficult to attribute to purely artificial heating. From approximately 16:25 UT onwards, the backscatter power is clearly associated with ionospheric pumping and remains relatively constant despite the pump beam direction changing. This indicates that striations are forming and they are growing to saturation. Wright et al. () showed that striations grow to saturation rapidly and once in a preconditioned ionosphere, as is the case here, they are maintained for very low pump powers. The consequence of this is that striations are saturated for all pumping directions, yet the optical emission intensity varies strongly with aspect angle. This suggests that the suprathermal electron acceleration mechanism relies on pump power being directed along the striations which maximises when the pump beam is pointed along the magnetic field-aligned direction.
Figure 5 shows four DASI images taken in the last 10 s of pump on for the cycle at 16:30 UT, from top to bottom, pump directions of −12°, −6°, vertical and +6° N. The +12° N position has not been included due to its similarity to +6° N. The red dotted lines in the left column of images show the position of the pump beam in 1° steps. The right column shows the optical intensity taken as a vertical cut through the image in 0.1° steps (blue line) and the pump beam ERP on the ground in the corresponding direction (green line). The red solid line shows the magnetic field line direction. The horizontal displacement between EISCAT and Skibotn and the pump wave reflection altitude have been taken into account. The pump power maximises in the pointing direction of the pump beam as expected. The plots clearly highlight the angular offset between pump power and enhanced O(1D) optical emission intensity. When the pump beam is pointing −12° N, the optical emission pattern is almost symmetrical about the magnetic field line direction. For the −6° N and vertical positions, the optical emission pattern is not symmetrical about the magnetic zenith with an enhanced tail towards the northward direction.
The efficiency of O(1D) photon production as a function of pump power requires knowledge of the D-region absorption. A higher pump power undergoes greater self-induced absorption due to pump-enhanced D-region electron temperatures (Senior et al. ). Without the EISCAT radar available, the electron density or temperature was not measured during this experiment. Instead, we use the ionospheric model for the auroral zone (IMAZ) (Friedrich and Landauer ), which includes a D-region plasma density model. Using the D-region absorption model of Senior et al. (), we calculate the D-region electron temperature enhancement and determine that the pump wave absorption varied around 8 to 10 dB as the power in the magnetic field-aligned direction varied. Reducing the heater ERP by this absorption factor gives a reduced absorption-corrected ERP that would have to be transmitted from the ground if there was no D-region absorption present. The photon production efficiency is in the range 20 to 40 R/MW in the magnetic zenith, falling to below 10 R/MW for other beam positions where the highest intensity emissions were found displaced slightly away from the magnetic zenith. We note that our estimates are considerably greater than those by Pedersen et al. () (4 R/MW in the magnetic zenith and 1.5 R/MW in the vertical), presumably because they did not compensate for D-region absorption.
By varying the EISCAT heater beam-pointing direction, it has been shown that the artificial pump-induced optical emission intensity is highly dependent upon the angular distance from the magnetic zenith. The optical emission intensity is usually maximum near the magnetic field-aligned direction even when there is more pump power in other directions. These observations are consistent with previous results from HAARP (Pedersen et al. , ) and Sura (Grach et al., , ). These observations suggest that the mechanism which accelerates suprathermal electrons, believed to include upper-hybrid resonance, is aspect sensitive and more efficient parallel to the magnetic field line compared to the direction where most pump power is being transmitted. Our modelling, which takes into account D-region absorption of the HF pump wave, shows that the O(1D) emission intensity to pump power ratio in the magnetic zenith direction is 20- to 40-R/MW ERP, which is significantly greater than the estimate by Pedersen et al. ().
Using the CUTLASS radar, the coherent backscatter power from striations was observed to remain quasi-constant when varying the pump beam direction. This indicates that the pump beam generates upper-hybrid resonance, and the striations saturate, for all directions. This shows that the presence of striations, and by proxy upper-hybrid waves, is not sufficient to explain why high fluxes of suprathermal electrons are generated preferentially parallel to the magnetic field line direction. The mechanism for this angular sensitivity effect is still not understood.
Cooperative UK Twin-Located Auroral Sounding System
digital all-sky imager
effective radiated power
parametric decay instability
stimulated electromagnetic emissions
thermal parametric instability
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EISCAT is an international association supported by research organisations in China (CRIRP), Finland (SA), Japan (NIPR and STEL), Norway (NFR), Sweden (VR) and UK (NERC). MJK was supported by the National Institute for Polar Research in the form of a visiting professorship.
The authors declare that they have no competing interests.
MJK conceived the experiment, collected the optical data and wrote the manuscript. CB analysed the data and produced the figures. MTR operated the ionospheric pump facility and analysed the ionosonde data. TKY provided the radar data. YO assisted with drafting and revising the manuscript. All authors read and approved the final manuscript.