Bibliography
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Found 133 entries in the Bibliography.
Showing entries from 101 through 133
| 2014 |
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Configuration of the local interstellar magnetic field Frisch, Priscilla; Andersson, B; Berdhyugin, A; Funsten, HO; DeMajistre, R; Magalhaes, A; McComas, D; , Piirola; Schwadron, N; Seriacopi, D; , others; Published by: Published on: |
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Predictability and Ensemble Modeling of the Space-Atmosphere Interaction Region Matsuo, Tomoko; Fuller-Rowell, Timothy; Akmaev, Rashid; Wang, Houjun; Fang, Tzu-Wei; Ide, Kayo; Kleist, Daryl; Whitaker, JS; Yue, Xinan; Codrescu, Mihail; , others; Published by: Published on: |
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Kuzmin, AK; Merzlyi, AM; Shadrin, DG; Yu, Potanin; Banshchikova, MA; Chuvashov, IN; Published by: Published on: |
| 2013 |
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On the fast zonal transport of the STS-121 space shuttle exhaust plume in the lower thermosphere Meier et al. (2011) reported rapid eastward transport of the STS-121 space shuttle (launch: July 4, 2006) main engine plume in the lower thermosphere, observed in hydrogen Lyman α images by the GUVI instrument onboard the TIMED satellite. In order to study the mechanism of the rapid zonal transport, diagnostic tracer calculations are performed using winds from the Thermosphere Ionosphere Mesosphere Electrodynamics General Circulation Model (TIME-GCM) simulation of July, 2006. It is found that the strong eastward jet at heights of 100\textendash110\ km, where the exhaust plume was deposited, results in a persistent eastward tracer motion with an average velocity of 45\ m/s. This is generally consistent with, though faster than, the prevailing eastward shuttle plume movement with daily mean velocity of 30\ m/s deduced from the STS-121 GUVI observation. The quasi-two-day wave (QTDW) was not included in the numerical simulation because it was found not to be large. Its absence, however, might be partially responsible for insufficient meridional transport to move the tracers away from the fast jet in the simulation. The current study and our model results from Yue and Liu (2010) explain two very different shuttle plume transport scenarios (STS-121 and STS-107 (launch: January 16, 2003), respectively): we conclude that lower thermospheric dynamics is sufficient to account for both very fast zonal motion (zonal jet in the case of STS-121) and very fast meridional motion to polar regions (large QTDW in the case of STS-107). Yue, Jia; Liu, Han-Li; Meier, R.R.; Chang, Loren; Gu, Sheng-Yang; , Russell; Published by: Journal of Atmospheric and Solar-Terrestrial Physics Published on: Jan-03-2013 YEAR: 2013 DOI: 10.1016/j.jastp.2012.12.017 |
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Global Navigation Satellite System (GNSS) based radio occultation (RO) technique has shown powerful ability in ionospheric electron density profiling in the past decade. The most frequently used Abel inversion method in electron density retrieval has some biases because of the used spherical symmetry assumption. Our previous series simulations and evaluations mainly concentrated in the middle and low latitude regions have shown some systematical bias especially in lower altitude of low latitude region. However, the RO derived electron density quality in the high latitude and polar region is rarely investigated and not quantitatively clear yet. In this study, the Abel inversion error over high latitude and polar regions are systematically investigated for the first time based on NCAR-TIEGCM simulations and real data evaluations. The TIMED data driven NCAR-TIEGCM modeled electron density during 2008 are used to simulate the COSMIC RO events. The Abel inversion error can then be estimated by comparing Abel retrievals from TIEGCM simulated occultation with the original TIEGCM simulations. The Abel inversion can reproduce the season, altitude, latitude, and local time variation patterns of electron density and auroral zone electron density nighttime enhancement well in high latitude and polar region. The Abel inversion tends to underestimate the electron density in the auroral zone and overestimate it on both the equatorward and poleward sides of the auroral zone. As simulated by the TIEGCM model, the significant relative error (\>25\%) mainly occurs in lower altitude (\<250\ km) inside and around auroral zone region. Above 250\ km, the relative error mostly is less than 25\%. Specifically, RMSE (root mean square error) of NmF2 error from simulation is \~8.5\%. The Abel error under real ionosphere situation would be worse because the ionosphere could be more complicated and noisier than the model simulation. The error distribution and its seasonal, local time and latitude variations can be explained by the spherical symmetry assumption used in the Abel inversion associated with the corresponding ionospheric electron density variations. The comparisons between PFISR and COSMIC RO electron density during 2007\textendash2011 and some previous validation studies agree well with our simulation results. We hope these results can stimulate more studies in high latitude ionospheric research using RO data. Yue, Xinan; Schreiner, William; Kuo, Ying-Hwa; Wu, Qian; Deng, Yue; Wang, Wenbin; Published by: Journal of Atmospheric and Solar-Terrestrial Physics Published on: 06/2013 YEAR: 2013 DOI: 10.1016/j.jastp.2013.03.009 Abel inversion; AURORA; COSMIC; Electron density; GNSS radio occultation; TIEGCM |
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The global configuration of the geomagnetic field shows that the maximum east-west difference in geomagnetic declination of northern middle latitude lies in the US region (~32\textdegree), which produces the significant ionospheric east-west coast difference in terms of total electron content first revealed by Zhang et al. (2011). For verification, it is valuable to investigate this feature over the Far East area, which also shows significant geomagnetic declination east-west gradient but smaller (~15\textdegree) than that of the US. The current study provides evidence of the longitudinal change supporting the thermospheric zonal wind mechanism by examining the climatology of peak electron density (NmF2), electron density (Ne) of different altitudes in the Far East regions with a longitude separation of up to 40\textendash60\textdegree based on ground ionosonde and space-based measurements. Although the east-west difference (Rew) over the Far East area displays a clear diurnal variation similar to the US feature, that is negative Rew (West Ne \> East Ne) in the noon and positive at evening-night, the observational results reveal more differences including: (1) The noontime negative Rew is most pronounced in April\textendashJune while in the US during February\textendashMarch. Thus, for the late spring and summer period negative Rew over the Far East region is more significant than that of the US. (2) The positive Rew at night is much less evident than in the US, especially without winter enhancement. (3) The magnitude of negative Rew tends to enhance toward solar maximum while in the US showing anticorrelation with the solar activity. The altitude distribution of pronounced negative difference (300\textendash400 km) moves upward as the solar flux increases and hence produces the different solar activity dependence at different altitude. The result in the paper is not simply a comparison corresponding to the US results but raises some new features that are worth further studying and improve our current understanding of ionospheric longitude difference at midlatitude. Zhao, Biqiang; Wang, Min; Wang, Yungang; Ren, Zhipeng; Yue, Xinan; Zhu, Jie; Wan, Weixing; Ning, Baiqi; Liu, Jing; Xiong, Bo; Published by: Journal of Geophysical Research: Space Physics Published on: 01/2013 YEAR: 2013 DOI: 10.1029/2012JA018235 geomagnetic declination; longitudinal variation; midlatitude ionosphere |
| 2012 |
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Dayside and nightside segments of a polar arc: The particle characteristics Park, J.; Min, K.; Parks, G.; Zhang, Y.; Lee, J.-J.; Baker, J.; Kim, H.; Hwang, J.; Yumoto, K.; Uozumi, T.; Lee, C.; Published by: Journal of Geophysical Research Published on: Jan-01-2012 YEAR: 2012 DOI: 10.1029/2011JA017323 |
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Optical observations of large-scale undulations in the 23rd cycle of solar activity A statistical analysis of observations of large-scale undulations during the 23rd cycle of solar activity was performed using optical data from two stations: Tixie (71.6\textdegreeN, 128.9\textdegreeE) and Zhigansk (66.8\textdegreeN, 123.4\textdegreeE). The total number of events recorded was 54 (43 events at Tixie and 11 at Zhigansk). The complete list of observed events is presented. The occurrence frequency of eveningside (17\textendash23 LT) undulations during the solar activity growth (1999) and decline (2003\textendash2005) phases tends to increase. Large-scale undulations were shown to be generated both on the equatorward boundary of the diffuse auroral zone and inside the diffuse zone, which does not necessarily occur during magnetic storms. Baishev, D.; Barkova, E.; Yumoto, K.; Published by: Geomagnetism and Aeronomy Published on: 04/2012 YEAR: 2012 DOI: 10.1134/S0016793212020028 |
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Study on Far Ultraviolet Imaging Spectrometer with Grating Dispersion for Atmosphere Remote Sensing The far ultraviolet imaging spectrometer with grating dispersion is mainly used in the detection of the ionosphere, thermosphere, auroral zone and glow zone. It is important for the study and application of the remote sensing of atmosphere in China. We designed two optical systems for the far ultraviolet imaging spectrometer, and obtained the plane grating structure prototype based on the principles of nadir and limb atmospheric sounding. The prototype working at the waveband of 120~180 nm consists of an off-axis parabolic mirror and an advanced Czerny-Turner spectral imaging system. The far ultraviolet response back-illuminating CCD is adopted as the detector. The corresponding experiment system was built to calibrate the basic performances of the spectrometer prototype. The spectral and spatial resolutions are 2 nm and 0.5 mrad respectively. The far ultraviolet imaging spectrometer prototype plays an important role in the study and application of atmospheric remote sensing. Yu, L.; Wang, S.; Lin, G.; Qu, Y.; Wang, L.; Published by: Spectroscopy and Spectral Analysis Published on: 03/2012 |
| 2011 |
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Latitudinal profile of UV nightglow and electron precipitations Dmitriev, A.V.; Yeh, H.-C.; Panasyuk, M.I.; Galkin, V.I.; Garipov, G.K.; Khrenov, B.A.; Klimov, P.A.; Lazutin, L.L.; Myagkova, I.N.; Svertilov, S.I.; Published by: Planetary and Space Science Published on: Jan-06-2011 YEAR: 2011 DOI: 10.1016/j.pss.2011.02.010 |
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Study on spectral broadband aberration-corrected imaging spectrometer for far-ultraviolet waveband Yu, Lei; Wang, Shurong; Qu, Yi; Lin, Guanyu; Published by: Optical Engineering Published on: Jan-06-2011 YEAR: 2011 DOI: 10.1117/1.3591947 |
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Global distributions of OH and O2 (1.27 μm) nightglow emissions observed by TIMED satellite Gao, Hong; Xu, JiYao; Chen, GuangMing; Yuan, Wei; Beletsky, A.; Published by: Science China Technological Sciences Published on: Jan-02-2011 YEAR: 2011 DOI: 10.1007/s11431-010-4236-5 |
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Yu, Lei; Wang, Shu-rong; Qu, Yi; Lin, Guan-yu; Published by: Applied optics Published on: |
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Study on spectrograph for ionosphere: a broadband imaging instrument prototype for far-ultraviolet Yu, Lei; Wang, Shu-rong; Lin, Guan-yu; Published by: Published on: |
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Global distributions of OH and O2 (1.27 $\mu$m) nightglow emissions observed by TIMED satellite In order to investigate the global distributions of temporal variations of OH and O 2 nightglow emissions, we statistically analyzed their variations with altitude, local time, and season Gao, Hong; Xu, JiYao; Chen, GuangMing; Yuan, Wei; Beletsky, AB; Published by: Science China Technological Sciences Published on: YEAR: 2011 DOI: https://doi.org/10.1007/s11431-010-4236-5 |
| 2010 |
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Fast meridional transport in the lower thermosphere by planetary-scale waves Published by: Journal of Atmospheric and Solar-Terrestrial Physics Published on: Jan-12-2010 YEAR: 2010 DOI: 10.1016/j.jastp.2010.10.001 |
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Electric fields and large-scale undulations in the evening sector of the diffuse auroral zone Baishev, D.; Barkova, E.; Stepanov, A.; Rich, F.; Yumoto, K.; Published by: Geomagnetism and Aeronomy Published on: Jan-02-2010 YEAR: 2010 DOI: 10.1134/S0016793210010056 |
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Correlation between the ionospheric WN4 signature and the upper atmospheric DE3 tide Wan, W.; Xiong, J.; Ren, Z.; Liu, L.; Zhang, M.-L.; Ding, F.; Ning, B.; Zhao, B.; Yue, X.; Published by: Journal of Geophysical Research Published on: Jan-01-2010 YEAR: 2010 DOI: 10.1029/2010JA015527 |
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Ionosphere around equinoxes during low solar activity Liu, Libo; He, Maosheng; Yue, Xin\textquoterightan; Ning, Baiqi; Wan, Weixing; Published by: Journal of Geophysical Research Published on: Jan-01-2010 YEAR: 2010 DOI: 10.1029/2010JA015318 |
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Program of transient UV event research at Tatiana-2 satellite Garipov, G.; Khrenov, B.; Klimov, P.; Morozenko, V.; Panasyuk, M.; Petrova, S.; Tulupov, V.; Shahparonov, V.; Svertilov, S.; Vedenkin, N.; Yashin, I.; Jeon, J.; Jeong, S.; Jung, A.; Kim, J.; Lee, J.; Lee, H; Na, G.; Nam, J.; Nam, S.; Park, I.; Suh, J.; Jin, J; Kim, M.; Kim, Y.; Yoo, B.; Park, Y.-S.; Yu, H.; Lee, C.-H.; Park, J.; Salazar, H.; Martinez, O.; Ponce, E.; Cotsomi, J.; Published by: Journal of Geophysical Research Published on: Jan-01-2010 YEAR: 2010 DOI: 10.1029/2009JA014765 |
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Program of transient UV event research at Tatiana-2 satellite Garipov, G.; Khrenov, B.; Klimov, P.; Morozenko, V.; Panasyuk, M.; Petrova, S.; Tulupov, V.; Shahparonov, V.; Svertilov, S.; Vedenkin, N.; Yashin, I.; Jeon, J.; Jeong, S.; Jung, A.; Kim, J.; Lee, J.; Lee, H; Na, G.; Nam, J.; Nam, S.; Park, I.; Suh, J.; Jin, J; Kim, M.; Kim, Y.; Yoo, B.; Park, Y.-S.; Yu, H.; Lee, C.-H.; Park, J.; Salazar, H.; Martinez, O.; Ponce, E.; Cotsomi, J.; Published by: Journal of Geophysical Research Published on: Jan-01-2010 YEAR: 2010 DOI: 10.1029/2009JA014765 |
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Optical Observations of the Eveningside Undulations during Solar Cycle 23 Baishev, DG; Barkova, ES; Fedorov, AA; Yumoto, K; Published by: Proc. 8th International Confer ence “Problems of Geocosmos Published on: |
| 2009 |
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This paper presents an investigation of geomagnetic storm effects in the equatorial and middle-low latitude F-region in the West Pacific sector during the intense geomagnetic storm on 13\textendash17 April, 2006. The event, preceded by a minor storm, started at 2130 UT on April 13 while interplanetary magnetic field (IMF)\ Bzcomponent was ready to turn southward. From 14\textendash17 the ionosphere was characterized by a large scale enhancement in critical frequency, foF2 (4\~6\ MHz) and total electron content (TEC) (\~30TECU, 1TECU=1\texttimes1016el/m2) followed by a long-duration negative phase observed through the simultaneous ionospheric sounding measurements from 14 stations and GPS network along the meridian 120\textdegreeE. A periodic wave structure, known as traveling ionospheric disturbances (TIDs) was observed in the morning sector during the initial phase of the storm which should be associated with the impulsive magnetospheric energy injection to the auroral. In the afternoon and nighttime, the positive phase should be caused by the combination of equatorward winds and disturbed electric fields verified through the equatorial F-layer peak height variation and modeled upward drift of Fejer and Scherliess [1997. Empirical models of storm time equatorial electric fields. Journal of Geophysical Research 102, 24,047\textendash24,056]. It is shown that the large positive storm effect was more pronounced in the Southern Hemisphere during the morning-noon sector on April 15 and negative phase reached to lower magnetic latitudes in the Northern Hemisphere which may be related to the asymmetry of the thermospheric condition during the storm. Zhao, Biqiang; Wan, Weixing; Liu, Libo; Igarashi, K.; Yumoto, K.; Ning, Baiqi; Published by: Journal of Atmospheric and Solar-Terrestrial Physics Published on: Jan-01-2009 YEAR: 2009 DOI: 10.1016/j.jastp.2008.09.029 |
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Ionospheric response to the geomagnetic storm on 13–17 April 2006 in the West Pacific region This paper presents an investigation of geomagnetic storm effects in the equatorial and middle-low latitude F-region in the West Pacific sector during the intense geomagnetic storm on 13–17 April, 2006. The event, preceded by a minor storm, started at 2130 UT on April 13 while interplanetary magnetic field (IMF) Bz component was ready to turn southward. From 14–17 the ionosphere was characterized by a large scale enhancement in critical frequency, foF2 (4∼6MHz) and total electron content (TEC) (∼30TECU, 1TECU=1×1016el/m2) followed by a long-duration negative phase observed through the simultaneous ionospheric sounding measurements from 14 stations and GPS network along the meridian 120°E. A periodic wave structure, known as traveling ionospheric disturbances (TIDs) was observed in the morning sector during the initial phase of the storm which should be associated with the impulsive magnetospheric energy injection to the auroral. In the afternoon and nighttime, the positive phase should be caused by the combination of equatorward winds and disturbed electric fields verified through the equatorial F-layer peak height variation and modeled upward drift of Fejer and Scherliess [1997. Empirical models of storm time equatorial electric fields. Journal of Geophysical Research 102, 24,047–24,056]. It is shown that the large positive storm effect was more pronounced in the Southern Hemisphere during the morning-noon sector on April 15 and negative phase reached to lower magnetic latitudes in the Northern Hemisphere which may be related to the asymmetry of the thermospheric condition during the storm. Zhao, Biqiang; Wan, Weixing; Liu, Libo; Igarashi, K.; Yumoto, K.; Ning, Baiqi; Published by: Journal of Atmospheric and Solar-Terrestrial Physics Published on: YEAR: 2009 DOI: https://doi.org/10.1016/j.jastp.2008.09.029 |
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UV radiation from the night-time atmosphere seen from the “Universitetsky-Tatiana” satellite Detectors on the "Universitetsky-Tatiana" satellite measured a smoothly varying intensity of UV radiation from the night-time atmosphere in the nadir direction and the intensity of the energetic electron flux at the orbit. At high latitudes the UV intensity in the auroral oval is interpreted as being due to electrons penetrating into the atmosphere. At middle latitudes the UV intensity is an order of magnitude less and more data are needed to reveal the origin of this radiation. Millisecond flashes of UV radiation were observed. Dmitriev, AV; Garipov, GK; Grigoryan, OR; Khrenov, BA; Klimov, PA; Lazutin, LL; Myagkova, IN; Petrov, AN; Petrov, VL; Panasyuk, MI; , others; Published by: Published on: YEAR: 2009 DOI: 10.1063/1.3137703 |
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Ionospheric response to the geomagnetic storm on 13—17 April 2006 in the West Pacific region Zhao, Biqiang; Wan, Weixing; Liu, Libo; Igarashi, K; Yumoto, K; Ning, Baiqi; Published by: Journal of Atmospheric and Solar-Terrestrial Physics Published on: |
| 2008 |
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Previous ground observations have revealed a correlation that exists between equatorial plasma bubbles, evening equatorial ionization anomaly (EIA), and prereversal E × B drift velocity using latitudinal arrays of ionospheric sounders, such as in the Indian and American regions. Besides the ground measurements, the space-based observations also provide a convenient way to study the global-scale variations. Li, Guozhu; Ning, Baiqi; Liu, Libo; Zhao, Biqiang; Yue, Xinan; Su, S-Y; Venkatraman, Sarita; Published by: Radio Science Published on: YEAR: 2008 DOI: 10.1029/2007RS003760 |
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Oscillations of the equatorward boundary of the ion auroral oval – radar observations Three SuperDARN radars in the afternoon-midnight sector of the auroral oval detected a boundary oscillation, originating near ∼1800 MLT sector. Analysis of the phase of the oscillations measured in three meridians indicates that the disturbance has a longitudinally (azimuthally) isolated source and away from which it propagates. The eastward and westward phase speeds are 2.6 and 3.6 km/s respectively and the period is roughly 28 minutes. An examination of the geo-synchronous magnetic field inclination also revealed oscillations similar to the oscillations of the boundary. Solar wind and IMF conditions were steady during the period except for variations of the IMF By component. The IMF By component showed variations similar to the oscillations in the boundary and the geo-synchronous magnetic field inclination. During reduced and negative IMF By, the boundary was moving equatorward, while during increased or positive IMF By it was moving poleward. The variations in the magnetic field inclination measured at geosynchronous orbit by the GOES satellites were consistent with these boundary motions: decreases (more stretched) and increases (more dipolar) in the inclination corresponded to equatorward and poleward moving boundaries, respectively. Polar cap convection also showed changes in the direction of the convection in response to the change in the IMF By component. Observed oscillation of the boundary can be explained by stretching of the tail field lines due to asymmetric merging associated with changes in the By component of the interplanetary magnetic field. Jayachandran, P.; Sato, N.; Ebihara, Y.; Yukimatu, A.; Kadokura, A.; MacDougall, J.; Donovan, E.; Liou, K.; Published by: Journal of Geophysical Research: Space Physics Published on: YEAR: 2008 DOI: https://doi.org/10.1029/2007JA012870 |
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Based on the DMSP F13 Satellite observations from 1995 to 2005, the longitudinal distributions of the electron temperature (Te) and total ion density (Ni) in the sunset equatorial topside ionosphere are examined. The results suggest that the longitudinal variations of both Te and Ni exhibit obvious seasonal dependence as follows: (1) wavenumber-four longitudinal structure in equinox, (2) three peaks structure in June solstice, and (3) two peaks structure in December solstice. Moreover, the longitudinal variations of Te and Ni show significant anti-correlation, and we speculate that the longitudinal variation of Te may result from that of Ni which can control Te through the electron cooling rate. The wavenumber-four longitudinal structures of both Te and Ni in equinox may relate to the eastward propagating zonal wavenumber-3 diurnal tide (DE3), which has effect on the amplitude of the daytime zonal electric field. The longitudinal variation of Te and Ni in the two solstices may be caused both by longitudinal variation of geomagnetic declination and DE3. Ren, Zhipeng; Wan, Weixing; Liu, Libo; Zhao, Biqiang; Wei, Yong; Yue, Xinan; Heelis, Roderick; Published by: Geophysical Research Letters Published on: YEAR: 2008 DOI: https://doi.org/10.1029/2007GL032998 |
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This dissertation focuses on the structure of the nonmigrating semidiurnal tide in the high latitude Mesosphere and Lower Thermosphere (MLT). Comparing the spatial structure and Published by: Published on: |
| 2007 |
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Ionospheric disturbances during the severe magnetic storm of November 7\textendash10, 2004 Grigorenko, E.; Lysenko, V.; Pazyura, S.; Taran, V.; Chernogor, L.; Published by: Geomagnetism and Aeronomy Published on: Jan-12-2007 YEAR: 2007 DOI: 10.1134/S0016793207060059 |
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Ionospheric disturbances during the severe magnetic storm of November 7—10, 2004 Grigorenko, EI; Lysenko, VN; Pazyura, SA; Taran, VI; Chernogor, LF; Published by: Geomagnetism and Aeronomy Published on: |
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GNSS-Based Radio Tomographic Studies of the Ionosphere at Different Latitudes We present the results of ionospheric imaging by the radio tomographic (RT) methods based on the Navigation Satellite Systems (GNSS). GNSS include the first-generation low orbiting (LO) systems (Tsikada, Transit, etc.) and second-generation high orbiting (HO) systems (GPS and GLONASS, which have been put in operation, and Galileo, BeiDou, and QZSS systems, which are currently under development in Europe, China, and Japan). Kunitsyn, Vyacheslav; Andreeva, Elena; Nesterov, Ivan; Tumanova, Yulia; Fedyunin, Yuri; Published by: Published on: |