Bibliography
Notice:
|
Found 24 entries in the Bibliography.
Showing entries from 1 through 24
2021 |
Inversion of Ionospheric O/N-2 by Using FY-3D Ionospheric Photometer Data Da-xin, Wang; Li-ping, Fu; Fang, Jiang; Nan, Jia; Tian-fang, Wang; Shuang-tuan, Dou; Published by: SPECTROSCOPY AND SPECTRAL ANALYSIS Published on: |
Inversion of Ionospheric O/N-2 by Using FY-3D Ionospheric Photometer Data Da-xin, Wang; Li-ping, Fu; Fang, Jiang; Nan, Jia; Tian-fang, Wang; Shuang-tuan, Dou; Published by: SPECTROSCOPY AND SPECTRAL ANALYSIS Published on: |
2020 |
Understanding the Behavior of the Ionosphere—Thermosphere—Mesosphere at Solar Minimum I Paxton, Larry; Deng, Yue; Liu, Huixin; Fang, Tzu-Wei; Published by: Published on: |
Plasma depletion bays in the equatorial ionosphere observed by FORMOSAT-3/COSMIC during 2007--2014 A new feature of plasma depletion bay (PDB) on the longitudinal structure over the equatorial and low latitudes is observed by the FORMOSAT-3/COSMIC (F3/C) electron density profiles. The existence of the PDB feature is confirmed by the OI 135.6 nm radiance from TIMED/GUVI, which together with F3/C electron density shows that one North PDB extending to the Southern Hemisphere prominently appears over Southwest America while three South PDBs extending to the Northern Hemisphere occur over North Atlantic, India Ocean, and Southeast Asia. Three-dimensional F3/C ionospheric electron densities are further used to examine PDB structures at various local times, seasons, solar activities, and altitudes during 2007−2014. Chang, FY; Liu, JY; Fang, TW; Rajesh, PK; Lin, CH; Published by: Journal of Geophysical Research: Space Physics Published on: YEAR: 2020   DOI: 10.1029/2019JA027501 |
2019 |
As part of its International Capabilities Assessment effort, the Community Coordinated Modeling Center initiated several working teams, one of which is focused on the validation of models and methods for determining auroral electrodynamic parameters, including particle precipitation, conductivities, electric fields, neutral density and winds, currents, Joule heating, auroral boundaries, and ion outflow. Auroral electrodynamic properties are needed as input to space weather models, to test and validate the accuracy of physical models, and to provide needed information for space weather customers and researchers. The working team developed a process for validating auroral electrodynamic quantities that begins with the selection of a set of events, followed by construction of ground truth databases using all available data and assimilative data analysis techniques. Using optimized, predefined metrics, the ground truth data for selected events can be used to assess model performance and improvement over time. The availability of global observations and sophisticated data assimilation techniques provides the means to create accurate ground truth databases routinely and accurately. Robinson, Robert; Zhang, Yongliang; Garcia-Sage, Katherine; Fang, Xiaohua; Verkhoglyadova, Olga; Ngwira, Chigomezyo; Bingham, Suzy; Kosar, Burcu; Zheng, Yihua; Kaeppler, Stephen; Liemohn, Michael; Weygand, James; Crowley, Geoffrey; Merkin, Viacheslav; McGranaghan, Ryan; Mannucci, Anthony; Published by: Space Weather Published on: 01/2019 YEAR: 2019   DOI: 10.1029/2018SW002127 |
Robinson, Robert; Zhang, Yongliang; Garcia-Sage, Katherine; Fang, Xiaohua; Verkhoglyadova, Olga; Ngwira, Chigomezyo; Bingham, Suzy; Kosar, Burcu; Zheng, Yihua; Kaeppler, Stephen; , others; Published by: Space Weather Published on: |
Research Progress on On-Orbit Calibration Technology for Far Ultraviolet Payload Li-ping, Fu; Nan, Jia; Xiu-qing, Hu; Tian, Mao; Fang, Jiang; Yun-gang, Wang; Ru-yi, Peng; Tian-fang, Wang; Da-xin, Wang; Shuang-tuan, Dou; , others; Published by: Published on: |
Research Progress on On-Orbit Calibration Technology for Far Ultraviolet Payload Li-ping, Fu; Nan, Jia; Xiu-qing, Hu; Tian, Mao; Fang, Jiang; Yun-gang, Wang; Ru-yi, Peng; Tian-fang, Wang; Da-xin, Wang; Shuang-tuan, Dou; , others; Published by: Published on: |
2015 |
We analyze how the evening equatorial plasma vortex and the prereversal enhancement (PRE) of the vertical drift are influenced by the distributions of conductivity in the E and F regions in relation to the wind, through numerical simulations with the thermosphere-ionosphere-electrodynamics general circulation model coupled with the global ionosphere-plasmasphere model. The nightside electric potential satisfies an approximate minimization principle that unifies the connection of the horizontal and vertical components of plasma convection to the wind and conductivity distributions. The relative roles of E and F region conductivities on the convection and current closure are clarified. Evening time F region zonal winds at latitudes that encompass the equatorial ionization anomaly (EIA) region provide the main energy source to drive the convection, including the PRE. The E region helps regulate both the meridional and the zonal convection through drag on the meridional convection associated with Cowling current. For large nighttime E region conductivities, additional drag on the zonal convection comes from the Pedersen conductance. The minimization principle favors meridional plasma inflow to the EIA region from lower rather than higher magnetic apex heights, so long as the E region Cowling conductance is not too large. This upward/poleward inflow maximizes on field lines that traverse the lower F layer near the equatorward edge of the EIA region, producing a PRE with maximum vertical velocity within the equatorial F layer. Published by: Journal of Geophysical Research: Space Physics Published on: 03/2015 YEAR: 2015   DOI: 10.1002/2014JA020935 equatorial ionosphere convection; night-time ionization; pre-reversal enhancement |
2014 |
Solar filament impact on 21 January 2005: Geospace consequences On 21 January 2005, a moderate magnetic storm produced a number of anomalous features, some seen more typically during superstorms. The aim of this study is to establish the differences in the space environment from what we expect (and normally observe) for a storm of this intensity, which make it behave in some ways like a superstorm. The storm was driven by one of the fastest interplanetary coronal mass ejections in solar cycle 23, containing a piece of the dense erupting solar filament material. The momentum of the massive solar filament caused it to push its way through the flux rope as the interplanetary coronal mass ejection decelerated moving toward 1 AU creating the appearance of an eroded flux rope (see companion paper by Manchester et al. (2014)) and, in this case, limiting the intensity of the resulting geomagnetic storm. On impact, the solar filament further disrupted the partial ring current shielding in existence at the time, creating a brief superfountain in the equatorial ionosphere\textemdashan unusual occurrence for a moderate storm. Within 1 h after impact, a cold dense plasma sheet (CDPS) formed out of the filament material. As the interplanetary magnetic field (IMF) rotated from obliquely to more purely northward, the magnetotail transformed from an open to a closed configuration and the CDPS evolved from warmer to cooler temperatures. Plasma sheet densities reached tens per cubic centimeter along the flanks\textemdashhigh enough to inflate the magnetotail in the simulation under northward IMF conditions despite the cool temperatures. Observational evidence for this stretching was provided by a corresponding expansion and intensification of both the auroral oval and ring current precipitation zones linked to magnetotail stretching by field line curvature scattering. Strong Joule heating in the cusps, a by-product of the CDPS formation process, contributed to an equatorward neutral wind surge that reached low latitudes within 1\textendash2 h and intensified the equatorial ionization anomaly. Understanding the geospace consequences of extremes in density and pressure is important because some of the largest and most damaging space weather events ever observed contained similar intervals of dense solar material. Kozyra, J.; Liemohn, M.; Cattell, C.; De Zeeuw, D.; Escoubet, C.; Evans, D.; Fang, X.; Fok, M.-C.; Frey, H.; Gonzalez, W.; Hairston, M.; Heelis, R.; Lu, G.; Manchester, W.; Mende, S.; Paxton, L.; Rastaetter, L.; Ridley, A.; Sandanger, M.; Soraas, F.; Sotirelis, T.; Thomsen, M.; Tsurutani, B.; Verkhoglyadova, O.; Published by: Journal of Geophysical Research: Space Physics Published on: 07/2014 YEAR: 2014   DOI: 10.1002/2013JA019748 cold dense plasma sheet; Equatorial anomaly; magnetotail; precipitation; prompt penetration electric field; solar filament |
Ionization due to electron and proton precipitation during the August 2011 storm The parameterizations of monoenergetic particle impact ionization in Fang et al. (2010) (Fang2010) and Fang et al. (2013) (Fang2013) are applied to the complex energy spectra measured by DMSP F16 satellite to calculate the ionization rates from electron and ion precipitations for a Northern Hemisphere pass from 0030 UT to 0106 UT on 6 August 2011. Clear enhancement of electron flux is found in the polar cap. The mean electron energy in the polar cap is mostly above 100 eV, while the mean energy in the auroral zone is typically above 1 keV. At the same time, F16 captures a strong Poynting flux enhancement in the polar cap, which is comparable to those in the auroral zone. The particle impact ionization rates using Fang2010 and Fang2013 parameterizations show clear enhancement at F region altitudes mainly due to the low-energy precipitating electrons, peaking probably in the cusp but also showing enhanced levels throughout most of the polar cap region. The general circulation models (GCMs), National Center for Atmospheric Research Thermosphere-Ionosphere-Electrodynamics General Circulation Model, and Global Ionosphere-Thermosphere Model, using their default empirical formulations of particle impact ionization, do not capture the observed features shown in the total particle ionization rate applying the Fang2010 and Fang2013 parameterizations to DMSP measurements. The difference between GCM simulations and Fang2010 and Fang2013 applied to DMSP data is due to the difference of both the inputs to the models and the parameterization of the ionization rates. Huang, Yanshi; Huang, Cheryl; Su, Yi-Jiun; Deng, Yue; Fang, Xiaohua; Published by: Journal of Geophysical Research: Space Physics Published on: 04/2014 YEAR: 2014   DOI: 10.1002/2013JA019671 Fang 2010 parameterization; Fang 2013 parameterization; particle impact ionization; polar cap |
Comparative studies of theoretical models in the equatorial ionosphere Fang, Tzu-Wei; Anderson, David; Fuller-Rowell, Tim; Akmaev, Rashid; Codrescu, Mihail; Millward, George; Sojka, Jan; Scherliess, Ludger; Eccles, Vince; Retterer, John; , others; Published by: Modeling the ionosphere—thermosphere system Published on: |
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: |
2012 |
Ionosphere response to recurrent geomagnetic activity in 1974 Fang, Tzu-Wei; Forbes, Jeffrey; Published by: Journal of Geophysical Research Published on: Jan-01-2012 YEAR: 2012   DOI: 10.1029/2011JA017017 |
2010 |
Equatorial-PRIMO (Problems Related to Ionospheric Models and Observations) Fang, T; Anderson, DN; Fuller-Rowell, TJ; Akmaev, RA; Codrescu, M; Millward, GH; Sojka, JJ; Scherliess, L; Eccles, JV; Retterer, JM; , others; Published by: Published on: |
Kozyra, JU; Brandt, PC; Cattell, CA; Clilverd, M; de Zeeuw, D; Evans, DS; Fang, X; Frey, HU; Kavanagh, AJ; Liemohn, MW; , others; Published by: Published on: |
2009 |
The causal link of the DE-3 tide, vertical drift, and plasma density Kil, Hyosub; Talaat, Elsayed; Paxton, Larry; Fang, Tzu-Wei; Oh, Seung-Jun; Published by: Published on: |
Global Ionospheric Structure Imaged by FORMOSAT-3/COSMIC: Early Results. A new era of study ing the ion o spheric space weather ef fects has come af ter launch of the in no va tive sat el lite con stel la tion, named as Formosa Sat el lite 3 or Con stel la tion Ob Lin, Chien-Hung; Liu, Jann-Yenq; Hsiao, Chun-Chieh; Liu, Chao-Han; Cheng, Chio-Zong; Chang, Po-Ya; Tsai, Ho-Fang; Fang, Tzu-Wei; Chen, Chia-Hung; Hsu, Mei-Lan; Published by: Terrestrial, Atmospheric \& Oceanic Sciences Published on: |
2007 |
Motions of the equatorial ionization anomaly crests imaged by FORMOSAT-3/COSMIC Lin, C.; Liu, J; Fang, T.; Chang, P; Tsai, H.; Chen, C.; Hsiao, C.; Published by: Geophysical Research Letters Published on: Jan-01-2007 YEAR: 2007   DOI: 10.1029/2007GL030741 |
Lin, C.; Wang, W.; Hagan, M.; Hsiao, C.; Immel, T.; Hsu, M.; Liu, J; Paxton, L.; Fang, T.; Liu, C.; Published by: Geophysical Research Letters Published on: Jan-01-2007 YEAR: 2007   DOI: 10.1029/2007GL029265 |
2006 |
Kozyra, J.; Crowley, G.; Emery, B.; Fang, X.; Maris, G.; Mlynczak, M.; Niciejewski, R.; Palo, S.; Paxton, L.; Randall, C.; Rong, P.-P.; Russell, J.; Skinner, W.; Solomon, S.; Talaat, E.; Wu, Q.; Yee, J.-H.; Published by: Published on: YEAR: 2006   DOI: 10.1029/GM16710.1029/167GM24 |
2005 |
Kozyra, JU; Crowley, G; Emery, BA; Fang, XH; Hagan, ME; Lu, G; Mlynczak, MG; Niciejewski, RJ; Palo, SE; Paxton, LJ; , others; Published by: Published on: |
2004 |
Quantification of the spreading effect of auroral proton precipitation A three-dimensional Monte Carlo model has been developed to study the transverse beam spreading effect of incident energetic auroral protons during their precipitation in the Earth\textquoterights upper atmosphere. Energetic protons with an isotropic angular distribution are injected at 700 km altitude. Two types of incident energy spectra, a monoenergetic and a Maxwellian distribution, are considered. Interaction of fast particles with a three-species atmosphere (O, N2, and O2) is included through charge exchange, electron stripping, ionization, excitation, and elastic scattering collisions. A uniform geomagnetic field is assumed in the model. The spreading effect is simulated for both a fine proton beam and a proton arc of longitudinal and latitudinal extent. It is found that the main dispersion region for a fine proton beam is located in the altitude range of around 250\textendash450 km, where the first few charge exchange collisions play a significant role. In the spreading study for a proton arc, we compare the numerical results with previous studies and give a convincing explanation by analyzing atmospheric scale heights and cross-section data. For the purpose of the model validity check, we make a comparison of the Monte Carlo simulation with observations and the results from other models. Fang, Xiaohua; Liemohn, Michael; Kozyra, Janet; Solomon, Stanley; Published by: Journal of Geophysical Research: Space Physics (1978\textendash2012) Published on: YEAR: 2004   DOI: 10.1029/2003JA010119 |
2002 |
Kozyra, JU; Baker, DN; Crowley, G; Evans, DS; Fang, X; Frahm, RA; Kanekal, SG; Liemohn, MW; Lu, G; Mason, GM; , others; Published by: Published on: |
1