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1 Click Here for Full Article GEOPHYSICAL RESEARCH LETTERS, VOL. 37,, doi: /2010gl042684, Model for artificial ionospheric duct formation due to HF heating 2 G. M. Milikh, 1 A. G. Demekhov, 2 K. Papadopoulos, 1 A. Vartanyan, 1 J. D. Huba, 3 3 and G. Joyce 4 4 Received 28 January 2010; revised 22 February 2010; accepted 26 February 2010; published XX Month [1] Strong electron heating by the injection of highly 6 powerful HF waves can lead to the formation of 7 ionospheric plasma density perturbations that stretch along 8 the magnetic field lines. Those density perturbations can 9 serve as ducts for guiding natural and artificial ELF/VLF 10 waves. This paper presents a theoretical model of duct 11 formation due to HF heating of the ionosphere. The model 12 is based on the modified SAMI2 code, and is validated by 13 comparison with two well documented experiments. One 14 experiment, conducted at the SURA heating facility, used 15 the low orbit satellite DEMETER as a diagnostic tool to 16 measure the electron and ion temperature and density along 17 the overflying satellite orbit close to the magnetic zenith of 18 the HF heater. The second experiment, conducted at the 19 EISCAT HF facility and diagnosed by the EISCAT 20 Incoherent Scatter Radar, measured the vertical profiles of 21 the electron and ion temperature between km. The 22 model agrees well with the observations, and provides a 23 new understanding of the processes during ionospheric 24 modification. Citation: Milikh, G. M., A. G. Demekhov, 25 K. Papadopoulos, A. Vartanyan, J. D. Huba, and G. Joyce (2010), 26 Model for artificial ionospheric duct formation due to HF heating, 27 Geophys. Res. Lett., 37,, doi: /2010gl Introduction 29 [2] It is well known that the presence of field aligned 30 density structures plays a critical role in the propagation of 31 whistler waves in the ionosphere. The density structures 32 serve as ducts for VLF/ELF waves since the density gradient 33 perpendicular to the magnetic field can lead to their total 34 internal reflection [Streltsov et al., 2006]. Such density 35 structures have often been observed [Carpenter et al., 2002] 36 to extend over distances covering entire magnetic field lines. 37 They are known to trap and guide whistler mode waves 38 between conjugate regions [e.g., Koons, 1989]. 39 [3] The possibility for creating such trans hemispheric 40 ducts artificially was discussed by Perrine et al. [2006], 41 where a 1D model which simulates the plasma along an 42 entire magnetic dipole field line was used. It was shown that 43 long term continuous HF heating of the F region by powerful 44 ionospheric heaters, such as HAARP, generates a strong 45 thermal wave in the ionospheric and magnetospheric plasma. 46 The thermal wave propagates along the magnetic field line through the topside ionosphere and magnetosphere, driving 55 ion outflows, displacing the ambient plasma and leading to 56 the formation of density ducts that stretch along the mag- 57 netic field line to the conjugate point. We have recently 58 generalized the previous 1D computational model to a 2D 59 model by incorporating simulations of the plasma in the 60 latitudinal direction. The new model allows one to describe 61 the ionospheric parameters in both vertical and latitudinal 62 directions with much better resolution than the old one. 63 Therefore the new model allows for close and useful com- 64 parisons with data obtained by radars and satellites that the 65 old model does not allow. The key objective of this paper is 66 to validate this new model based on SAMI2. To accomplish 67 this we will check the model against two recent well diag- 68 nosed experiments which detected large scale ducts caused 69 by the HF heating. One experiment was conducted at the 70 SURA heating facility and used the low orbit satellite 71 DEMETER [Berthelier et al., 2006a, 2006b] as a diagnostic 72 tool [Frolov et al., 2008] to measure the electron and ion 73 temperature and density along the satellite orbit close to the 74 magnetic zenith of the HF heater. Another heating experi- 75 ment, conducted at the EISCAT HF facility and diagnosed 76 by the EISCAT Incoherent Scatter Radar (ISR) [Rietveld et 77 al., 2003], measured the vertical profiles of the electron and 78 ion temperature between km. 79 [4] The letter is organized as following: the next section 80 describes the numerical model applied. In the discussion 81 section the model output is compared with the EISCAT radar 82 and DEMETER observations followed by conclusions Numerical Model of Formation of the Artificial 84 Ducts 85 [5] The theoretical/computational model is based on the 86 SAMI2 code developed at the Naval Research Laboratory 87 [Huba et al., 2000]. The code is a Eulerian grid based code, 88 which describes an ionosphere made up of seven ion species. 89 The equations of continuity and momentum are solved for 90 the electrons and each ion species, with the temperature 91 equation solved for the electrons and H +, He +, and O + 92 species. The electron density is determined on the basis of 93 charge neutrality. The code includes E B drift of the field 94 lines with frozen in plasma (in altitude and longitude), an 95 empirical neutral atmosphere model, horizontal winds, 96 photo deposition into the ionosphere, ion chemistry models, 97 and ion inertia. This inclusion of ion inertia is critical since it 98 allows for the study of sound wave propagation in the 99 plasma. The SAMI2 model is inter hemispheric and can 100 simulate the plasma along the entire dipole magnetic field line 101 (for the geometry of the model see Perrine et al. [2006]). The 102 most recent version of the SAM12 code (release 0.98) which 103 allows description of processes at high latitudes was used 104 here. HF heating of the ionosphere is a complex phenomenon Department of Physics and Department of Astronomy, University of Maryland, College Park, Maryland, USA. 2 Institute of Applied Physics, Russian Academy of Sciences, Nizhny Novgorod, Russia. 3 Naval Research Laboratory, Washington, DC, USA. 4 Icarus Research, Inc., Bethesda, Maryland, USA. Copyright 2010 by the American Geophysical Union /10/2010GL of5
2 106 It begins with the HF absorption which pumps the iono- 107 spheric turbulence that in turn generates the plasma heating 108 [Gurevich et al., 1996; Gustavsson et al., 2001]. Since the 109 SAMI2 code does not consider wave propagation and ab- 110 sorption we introduced in the model a flexible source of 111 electron heating, as we did it in an earlier paper by Perrine et 112 al. [2006]. This source of the electron heating was presented 113 in the form of localized heating rate per electron q ¼ P fðx; zþ ¼ 260 PMW ð Þ 10km 300km 2 Vn e a z up ð1þ 1 tan 2 fðx; zþk=s 114 Here P is the power of the HF heater, V is the volume of the 115 HF absorbed region, n e is the electron density in this region, 116 while m is the absorption efficiency. f(x, z) describes the 117 spatial distribution of the HF beam power density taken as z zup fðx; zþ ¼ e ð Þ2 =a 2 e ½ Š ð2þ ln 2 ð x x0 Þ2 =b The center of the heated region is taken at the upper hybrid 119 altitude z up. Furthermore, b is the half power beam width near 120 the upper hybrid point. The HF irradiated spot is taken as a 121 circle centered at x o having the angular half widths Q so that 122 b = z up tan, and the HF irradiated volume is V = pab Finally, it is assumed that electron heating occurs in an al- 124 titude range having the vertical extent a between the wave 125 reflection point and the upper hybrid height, which is 126 dominated by the anomalous absorption [Gurevich et al., ]. 128 [6] In this paper we will model the ionospheric conditions 129 at Tromso during 10/07/99 at the time of the EISCAT 130 experiment [Rietveld et al., 2003]. We therefore use in the 131 SAMI2 code the corresponding A p and F 10.7 indexes, and 132 assume that the heating began 10/7/99 at 19:24 UT. The 133 radiated HF power was 960 kw, the half power beam 134 width was 12, and the facility was operated at a frequency 135 of 4.5 MHz. Furthermore, for the unperturbed profile of 136 the electron density we find that the reflection height for 137 the 4.5 MHz frequency is located at 280 km, while the 138 upper hybrid height is at about 10 km below. Thus the 139 vertical extend of the anomalous absorption region is taken 140 as a = 10 km. 141 [7] Before proceeding we should caution the reader on the 142 timescale of model validity. The model neglects the hori- 143 zontal transport caused by the E B drift, which has a time 144 scale t dr = b/v dr, where v dr is the drift velocity and b is the 145 horizontal scale of the heated region. Taking into account 146 that the Tromso HF heater has a half power beam width of and that the electron heating occurs at an altitude of km, we obtain that the horizontal scale of the heated 149 region is b = 60 km. Moreover during the time of the dis- 150 cussed experiments the detected drift velocity was m/s [Rietveld et al., 2003]. Thus the E B drift led to 152 energy loss followed by the reduction of the heating effect 153 on a time scale of minutes Simulation Procedure 155 [8] The code starts up from empirically determined initial 156 conditions 24 hours before the specific heating time, and 157 runs for 24 hours of world clock time. This practice allows 158 the system to relax to ambient conditions, and reduces noise in the system due to the initialization. Furthermore, the neutral density model was adjusted so that the computed f 0 F 2 peak matched the observed. Then the artificial heater turns on and begins to pump energy into the electrons, using the specified parameters for that run. Artificial heating continues for some time continuously pumping energy into the electrons at the specified altitude, and the perturbations in ion and electron properties are tracked as they travel along the field line. Then the heater switches off, allowing the ionosphere to relax back to ambient conditions. The latter may also vary according to the natural factors which determine the ionosphere dynamics. This procedure minimizes noise due to the initialization and allows for the perturbations in the ionosphere to travel along the field lines, and the ionosphere to relax following strong heating. It describes the plasma response to the removal of the artificial heating as well as to its application. [9] In order to isolate and measure the perturbations directly, a duplicate set of runs was made, identical to the run described, but with a different heating rate defined by factor q in equation (1). In addition, one run without artificial heating was performed. We refer to this as ambient or reference run, while those with artificial heating are heated runs. The ionosphere changes during a simulation due to natural causes, so the perturbations in the heated runs due to artificial heating would not be easily identifiable on their own. But since the same natural variations are present in the ambient data, scaling (or subtracting) by the ambient data provides a simple way to decouple the natural variations from the heater induced perturbations. 3. Discussion 3.1. Comparison With Tromso Experiments [10] In order to reproduce results of the ISR observations made at Tromso we conducted some runs using the specified conditions at Tromso 10/7/99. Namely, we considered the index A p = 5, and that the HF heating began at 19:24 UT. For the specified heater and antenna characteristics at EISCAT equation (1) gives that q = 12,400 m, K/s. In our runs the heating rate varied in the range 2,000 8,000 K/s which corresponds to the absorption efficiency m = Note that Gustavsson et al. [2001] used the radar data collected during the heating experiments at Tromso to estimate the heating rate per electron as 3,000 K/s. This value corresponds to the absorption efficiency m = 0.25, which is within the range of our estimates. [11] Figure 1 shows the height profile of the electron density normalized to its ambient value computed at different times for a given pumping rate q = 8,000 K/s which corresponds to an absorption efficiency m = The heating was switched on at 19:24:00 UT for 8 minutes. The traces labeled 1 to 3 correspond to times separated by 3 minutes starting at 19:25:46, i.e. 1 min and 46 s into the heating. The trace 4 corresponds to cooling over 2 minutes and 49 seconds. Figure 1 reveals that the electron heating increases the plasma pressure and thus pushes the plasma from the heated region along the magnetic field line. Consequently, the plasma density in the heated region drops by more than 20%, but on a timescale larger than 5 minutes, as shown by the trace 3. [12] Figure 2 shows the results of our model superimposed onto the observation results presented by Rietveld of5
![The trace 4 corresponds to cooling over 2 minutes and 49 seconds. 220 et al. [2003, Figure 3]. The latter were made by the EISCAT 221 ISR at 19:28 UT.](/docs-images/90/101792409/images/3-2.jpg "Figure 2 (left) shows the observed altitude 222 profile of the electron density (circles) and that computed by 223 the SAMI2 model (continuous trace) for 4 minutes in the 224 heating.")
3 Figure 1. The electron density normalized to its ambient value computed at different times for a pumping rate q = 8,000 K/s which corresponds to the absorption efficiency m = The heating was switched on at 19:24:00 UT for 8 minutes. The traces labeled 1 to 3 correspond to times separated by 3 minutes starting at 19:25:46, i.e. 1 min and 46 s into the heating. The trace 4 corresponds to cooling over 2 minutes and 49 seconds. 220 et al. [2003, Figure 3]. The latter were made by the EISCAT 221 ISR at 19:28 UT. Figure 2 (left) shows the observed altitude 222 profile of the electron density (circles) and that computed by 223 the SAMI2 model (continuous trace) for 4 minutes in the 224 heating. Figure 2 (middle) shows the observed ion temper- ature (circles) and electron temperature (crosses) along with 225 the three traces generated by SAM12 model. 226 [13] In order to improve agreement between the model 227 and observations the neutral density in the model was 228 adjusted so that the computed f o F 2 peak matches the ob- 229 Figure 2. (left) The observed altitude profile of the electron density (circles) and the one computed by SAMI2 (continuous trace) for the four minute time interval starting on at 10/07/99 at 19:24:00 UT. (middle) The observed ion temperature (circles) and electron temperature (crosses) along with the three traces generated by the SAMI2 model. The dashed, solid, and dotdashed line corresponds to the absorption efficiencies m = 0.16, 0.32 and 0.64 respectively. (right) The observed ion velocity (diamonds) along with the three traces which correspond to the computations made at m = 016, 0.32 and 0.64 (from left to right). 3of5
4 Figure 3. Relative changes in the density of O + ions computed for the two different absorption efficiencies m = 0.17 and The crosses show DEMETER observations reported by Frolov et al. [2008]. 230 servations. For this purpose we have reduced the density of 231 the atomic oxygen in the model by 50%. Such an approach is 232 justified by the fact that SAMI2 uses averaged model values 233 of the neutral density which may not very accurate. The 234 adjustment leads to significant changes in the electron 235 temperature and affects the vertical velocity only slightly. 236 The dashed, solid, and dot dashed lines in Figure 2 cor- 237 responds to the absorption efficiencies m = 0.16, 0.32 and , respectively. Note that the changes in m affect only 239 the values of electron temperature, while the ion temper- 240 ature remains unperturbed during a relatively short heating 241 pulse. Figure 2 (right) shows the observation of the ion 242 velocity (diamonds) along with the three traces which 243 correspond to the computations made at different absorp- 244 tion efficiencies m = 0.16, 0.32 and 0.64 (from the left to 245 right). Also, in this case the HF heating duration did not 246 exceed the time scale of E B drift and thus the energy 247 loss due to horizontal transport can be neglected. 248 [14] Figure 2 reveals that (1) HF heating with the absorp- 249 tion efficiencies m = drives perturbations of the 250 electron temperature in good agreement with those detected 251 by the ISR and (2) The computed ion velocity fits well with 252 the observations. Namely, it shows that the ion velocity is 253 negative below the heating region, and positive above it. A 254 strong electron heating increases the electron pressure and 255 pushes the plasma both down and upward from the heated 256 region. Thus below this region the ion velocity is negative 257 (downward directed), while above the region it is positive 258 (upward directed) and its value increases with altitude 259 since the plasma propagates in the ionosphere of decreas- 260 ing density Comparison With SURA Experiments 262 [15] Frolov et al. [2008] reported the detection of plasma 263 ducts by the DEMETER satellite overflying the SURA HF 264 heater. In fact, ducts were detected when the heater operated 265 at 4.3 MHz, and at ERP = 80 MW, while the half power 266 beam width was 12 on 05/01/06. The ionosphere was quiet, 267 Kp = 0, and the heating wave was reflected at 230 km, 268 below the f 0 F 2 peak. 269 [16] We conducted SAMI2 runs for this day for SURA 270 location (56 N, 46 E) using the specified characteristics 271 of the HF heater. The heating began 10 minutes before 272 the DEMETER overfly at 18:28:39 UT, and lasted for 15 minutes. Figure 3 shows the relative changes in the 273 density of O + ions computed for the two different pumping 274 rates q = 1,000 and 1,700 K/s which correspond to the 275 absorption efficiency m = 0.17 and 0.29 respectively. The 276 increase in O + density was then checked against the 277 DEMETER observations shown by crosses. The latter data 278 were derived from the DEMETER observations of the time 279 series of O + density [Frolov et al., 2008]. We converted 280 these data into the relative ion density by dividing them by 281 the value of the unperturbed O + density measured outside the 282 duct. In addition, we presented the relative O + density as a 283 function of latitude by taking into account the orbital velocity 284 v = 7 km/s of DEMETER. Figure 3 shows a good agreement 285 between the observations and model for the case of the 286 absorption efficiency m = Note that similar HF heating 287 experiments were conducted at HAARP using Demeter as a 288 diagnostic tool [Milikh et al., 2008] Concluding Remarks 290 [17] Recently modified SAMI2 numerical model was val- 291 idated by comparison with two well documented experi- 292 ments. One experiment, conducted at the SURA heating 293 facility, used the low orbit satellite DEMETER as a diag- 294 nostic tool to measure the electron and ion temperature and 295 density along the overflying satellite orbit close to the 296 magnetic zenith of the HF heater. The second experiment, 297 conducted at the EISCAT HF facility and diagnosed by the 298 EISCAT ISR, measured the vertical profiles of the electron 299 and ion temperature between km. The model 300 reproduces the observations with high accuracy, which 301 indicates its potential as a key tool for study of the arti- 302 ficial ducts, and to guide future observational campaigns. In 303 addition, the model predicts that the ionospheric HF heating 304 could produce strong perturbations of the plasma pressure 305 which will then transform into magnetic field perturbations 306 that could be detected by low orbit satellites having on board 307 magnetometers such as DMSP. Moreover by checking the 308 model results against the ISR or satellite made observations 309 one can assess efficiency of the duct production, namely what 310 fraction of the radio beam energy was pumped into the ducts. 311 [18] Acknowledgments. The work was supported by DARPA via a 312 subcontract N with BAE Systems. It was also supported by the 313 ONR grant NAVY.N C60 and by the ONR MURI grant 314 N The work of A.D. was also supported in part by the Russian 315 Academy of Sciences (the Program Plasma Processes in the Solar System ). 316 References 317 Berthelier, J. J., et al. (2006a), ICE, the electric field experiment on 318 DEMETER, Planet. Space Sci., 54, , doi: /j. 319 pss Berthelier, J. J., et al. (2006b), IAP, the thermal plasma analyzer on 321 DEMETER, Planet. Space Sci., 54, , doi: /j. 322 pss Carpenter, D. L., M. A. Spasojević, T. F. Bell, U. S. Inan, B. W. Reinisch, 324 I. A. Galkin, R. F. Benson, J. L. Green, S. F. Fung, and S. A. Boardsen 325 (2002), Small scale field aligned plasmaspheric density structures in- 326 ferred from the Radio Plasma Imager on IMAGE, J. Geophys. Res., (A9), 1258, doi: /2001ja Frolov, V. L., et al. 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