Bibliography

Notice:

Clicking on the title will open a new window with all details of the bibliographic entry.
Clicking on the DOI link will open a new window with the original bibliographic entry from the publisher.
Clicking on a single author will show all publications by the selected author.
Clicking on a single keyword, will show all publications by the selected keyword.

Found 130 entries in the Bibliography.

Showing entries from 101 through 130

2006

Investigating the state of the Sun-Earth system during extreme events: First science results of a worldwide online conference series

Kozyra, JU; Shibata, K; Fox, NJ; Basu, S; Coster, AJ; Davila, JM; Gopalswamy, N; Liou, K; Lu, G; Mann, IR; , others;

Published by: Published on:

YEAR: 2006 DOI:

Cluster observation of plasma flow reversal in the magnetotail during a substorm

Lui, ATY; Zheng, Y; Zhang, Y; Livi, S; Reme, H; Dunlop, MW; Gustafsson, Georg; Mende, SB; Mouikis, C; Kistler, LM;

Published by: Published on:

YEAR: 2006 DOI:

2005

Energy transport in the thermosphere during the solar storms of April 2002

Mlynczak, Martin; Martin-Torres, Javier; Crowley, Geoff; Kratz, David; Funke, Bernd; Lu, Gang; Lopez-Puertas, Manuel; Russell, James; Kozyra, Janet; Mertens, Chris; Sharma, Ramesh; Gordley, Larry; Picard, Richard; Winick, Jeremy; Paxton, L.;

Published by: Journal of Geophysical Research Published on: Jan-01-2005

YEAR: 2005 DOI: 10.1029/2005JA011141

Large-scale variations of the low-latitude ionosphere during the October\textendashNovember 2003 superstorm: Observational results

Lin, C.; Richmond, A.D.; Liu, J.Y.; Yeh, H.C.; Paxton, L.; Lu, G.; Tsai, H.F.; Su, S.-Y.;

Published by: Journal of Geophysical Research Published on: Jan-01-2005

YEAR: 2005 DOI: 10.1029/2004JA010900

Introduction to violent Sun-Earth connection events of October\textendashNovember 2003

The solar-terrestrial events of late October and early November 2003, popularly referred to as the Halloween storms, represent the best observed cases of extreme space weather activity observed to date and have generated research covering multiple aspects of solar eruptions and their space weather effects. In the following article, which serves as an abstract for this collective research, we present highlights taken from 61 of the 74 papers from the Journal of Geophysical Research, Geophysical Research Letters, and Space Weather which are linked under this special issue. (An overview of the 13 associated papers published in Geophysics Research Letters is given in the work of Gopalswamy et al. (2005a)).

Gopalswamy, N.; Barbieri, L.; Cliver, E.; Lu, G.; Plunkett, S.; Skoug, R.;

Published by: Journal of Geophysical Research Published on: 09/2005

YEAR: 2005 DOI: 10.1029/2005JA011268

coronal mass ejections; Geomagnetic storms; interplanetary shocks; solar energetic particles; Solar flares; superstorms

Introduction to violent Sun-Earth connection events of October\textendashNovember 2003

Gopalswamy, N.; Barbieri, L.; Cliver, E.; Lu, G.; Plunkett, S.; Skoug, R.;

Published by: Journal of Geophysical Research Published on: 09/2005

YEAR: 2005 DOI: 10.1029/2005JA011268

coronal mass ejections; Geomagnetic storms; interplanetary shocks; solar energetic particles; Solar flares; superstorms

Undulations on the equatorward edge of the diffuse proton aurora: TIMED/GUVI observations

Undulations on the equatorward edge of the diffuse proton aurora have been identified by using TIMED/GUVI auroral images in the far ultraviolet wavelengths. While undulations have been previously reported on the duskside (Lui et al., 1982), GUVI observations show the undulation also occurs in the dayside, nightside, and morningside. The GUVI proton auroral images provide direct optical evidence that the undulations occur in the proton aurora. It is also the first detection of the undulation in the dayside indicating strong convection shear in the region. The undulation in the nightside, a wavy structure in the whole diffuse proton aurora, is significantly different from those in the duskside and dayside. While almost all of the undulation events are observed during magnetic storms (Dst \< -60 nT), one exceptional case shows undulation in the dayside with Dst = 30 nT. However, the case is associated with a large solar wind speed (650 km/s) and a high dynamic pressure (14 nPa). Coincident DMSP SSIES observations suggest that both large ion drift velocity (\>1000 m/s) and strong velocity shear (\>0.1 s^-1) within the diffuse aurora oval are necessary conditions for the undulation to occur. The SSIES data also indicate the areas with large ion drift velocity and shear move to higher latitudes in the MLT sectors toward midnight. This may explain why the undulation is rarely detected in the nightside.

Zhang, Y.; Paxton, L.; Morrison, D.; T. Y. Lui, A.; Kil, H.; Wolven, B.; Meng, C.-I.; Christensen, A.;

Published by: Journal of Geophysical Research Published on: 09/2005

YEAR: 2005 DOI: 10.1029/2004JA010668

auroral undulation; K-H instability; Magnetic storm; plasma convection

Violent Sun-Earth Connection Events of October-November 2003-A09S28-Large-scale variations of the low-latitude ionosphere during the October-November 2003 superstorm

Lin, CH; RichmondJ Y Liu, AD; Yeh, HC; Paxton, LJ; Lu, G; Tsai, HF; Su, SY;

Published by: Journal of Geophysical Research-Part A-Space Physics Published on:

YEAR: 2005 DOI:

Large-scale variations of the low-latitude ionosphere during the October-–November 2003 superstorm: Observational results

The GPS-derived total electron content (TEC), ion drift measurements from the ROCSAT-1 spacecraft at around 600 km altitude, and far-ultraviolet airglow measured by the Global Ultraviolet Imager (GUVI) carried on board the NASA TIMED satellite are utilized for studying large disturbances of the low-latitude ionosphere during the October–November 2003 superstorm period. Two chains of GPS receivers, one in the American sector (∼70°W) and the other in the Asian/Australian sector (∼120°E), are used to simultaneously observe the daytime equatorial ionization anomaly (EIA) during the entire storm period. It is found from the GPS-TEC measurements that the EIA expanded to very high latitudes with large increases of TEC right after the storm started. The large expansion of the EIA was associated with strong upward E × B drifts measured from the Ionospheric Plasma and Electrodynamics Instrument (IPEI) on board the ROCSAT-1, providing evidence of a penetration electric field and a strong plasma fountain effect. Suppression of the EIA was observed during the storm recovery, associated with downward E × B drifts that were observed by the ROCSAT-1. Significant negative storm effects in the southern hemisphere were also observed in the GPS-TEC during the first day of the recovery phase. The areas of negative storm effects are in good agreement with reductions in the [O]/[N2] density ratio inferred from the ratio of OI (135.6 nm) to LBH emissions measured from GUVI. An enhancement of the EIA was observed on the day, 1 November, that the storm was about to fully recover.

Lin, C.; Richmond, A.; . Y. Liu, J; Yeh, H.; Paxton, L.; Lu, G.; Tsai, H.; Su, S.-Y.;

Published by: Journal of Geophysical Research: Space Physics Published on:

YEAR: 2005 DOI: https://doi.org/10.1029/2004JA010900

ionospheric disturbances; Magnetic storm; TEC enhancement

Seasonal and longitudinal variation of large-scale topside equatorial plasma depletions

We examine the large-scale properties of three classes of equatorial topside plasma depletions referred to as channels. In order of increasing zonal width and internal large-scale substructuring, we study simple channels, multichannels, and superchannels. We find that peaks in channel activity are centered on 0° (African sector) and 180° (Western Pacific sector). Superchannels are found to strongly dominate in the African sector, whereas simple and multichannels dominate the Pacific sector. Within the African sector, the relative proportions of the three channel classes remain stable in all seasons. In the Pacific sector, simple and multichannels are dominant in all seasons of activity, though small but significant seasonal variations in channel widths and spacings are seen. Structure at a zonal scale size of about 100 km is found to be present in all channels examined. Observational and model evidence suggests that 100-km density structure represents channels, such that all multichannels and superchannels consist of multiple contiguous simple channels. Since seeds that initiate channel formation necessarily influence large-scale channel features, we utilize our data to draw conclusions regarding bottomside seeding conditions in the various seasonal and longitudinal sectors. Specifically, we find that strong, long-wavelength (∼1000 km) seeds appear much more frequently in the African sector, resulting in the prevalence of superchannels there. When long-wavelength seeds appear in the Pacific sector, they result in periodic trains of simple and multichannels. A bottomside preseeded at a scale size near 100 km accounts for the ubiquity of 100-km scale size in the AE-E data.

Hei, M.; Heelis, R.; McClure, J.;

Published by: Journal of Geophysical Research: Space Physics Published on:

YEAR: 2005 DOI: https://doi.org/10.1029/2005JA011153

bubbles; equatorial plasma depletions; plumes

Auroral Undulations During Magnetic Storms: TIMED/GUVI Observations

Zhang, Y; Paxton, LJ; Morrison, D; Lui, T; Kil, H; Wolven, B; Meng, CI;

Published by: Published on:

YEAR: 2005 DOI:

Large-scale variations of the low-latitude ionosphere during the October—November 2003 superstorm: Observational results

Lin, CH; Richmond, AD; Liu, JY; Yeh, HC; Paxton, LJ; Lu, G; Tsai, HF; Su, S-Y;

Published by: Journal of Geophysical Research: Space Physics Published on:

YEAR: 2005 DOI:

Introduction to violent Sun-Earth connection events of October—November 2003

Gopalswamy, N; Barbieri, L; Cliver, EW; Lu, G; Plunkett, SP; Skoug, RM;

Published by: Journal of Geophysical Research: Space Physics Published on:

YEAR: 2005 DOI:

Introduction to violent Sun-Earth connection events of October—November 2003

Gopalswamy, N; Barbieri, L; Cliver, EW; Lu, G; Plunkett, SP; Skoug, RM;

Published by: Journal of Geophysical Research: Space Physics Published on:

YEAR: 2005 DOI:

A Virtual Metadata Generator for the TIMED Program

Morrison, D; Weiss, M; Daley, R; Immer, E; Hashemian, M; Nylund, S; Skura, J;

Published by: Published on:

YEAR: 2005 DOI:

Atmospheric Effects of Coronal Holes and Powerful High-Speed Solar Wind Streams in 2003 Observed by the TIMED Spacecraft

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:

YEAR: 2005 DOI:

CEDAR/TIMED: Thermospheric Vertical Wind Observations from Three Sites in the Northern Auroral Zone

Lummerzheim, D;

Published by: Published on:

YEAR: 2005 DOI:

2004

Contribution of proton precipitation to space-based auroral FUV observations

Imaging from space offers a unique way to access the global picture, and its temporal variability, of the particle energy input over the auroral ovals. Electron characteristics are inferred from the analysis of auroral images taken from space in two different spectral bands in UV or visible. Usually, only the electron component of the precipitation is considered, as most of the particle energy is carried by electrons. However, at some locations and certain times protons are a major energy source, that is, a major ionization and excitation source of the atmosphere. The response of POLAR/UVI, IMAGE/WIC and SI13, and TIMED/GUVI (used for retrieving the electron components) to proton precipitation is estimated. Secondary electrons produced within the proton beam also contribute to auroral emissions. Since they are less energetic than the secondary electrons produced in electron aurora, they have a different spectral signature. In addition, for a given energy flux, protons are usually more efficient at ionizing than electrons and yield larger values of the Pedersen ionospheric conductance. Therefore the difference between proton and electron aurora can lead to misinterpretation when brightness ratios are used to derive ionospheric conductances with parameterizations that are based on electron aurora. The validation and limitations of auroral analysis are discussed, especially at the equatorward edge of the afternoon oval, where protons are a significant energy source. In regions of \>4 keV electron precipitation, the presence of proton precipitation, even modest (\~10\%), yields a large underestimation of both the electron mean energy and the energy flux. Overall, the presence of proton precipitation yields a poor estimation of the electron mean energy. In proton-dominated aurora, the Pedersen and Hall conductances are always underestimated with a large discrepancy for POLAR/UVI. However, in location where the protons are not dominant and the electron precipitation is not too hard, it is legitimate to estimate the particle characteristics and ionospheric conductances from the FUV brightnesses assuming pure electron precipitation. This is true in particular for the period around midnight (1900\textendash0400 MLT), at a magnetic latitude of 65\textendash67\textdegree.

Galand, M.; Lummerzheim, D.;

Published by: Journal of Geophysical Research Published on: 03/2004

YEAR: 2004 DOI: 10.1029/2003JA010321

auroral protons; FUV

IMAGE-FUV observations of the October-November 2003 flare and magnetic storm effects on Earth

Immel, TT; Ostgaard, N; Strickland, DJ; Frey, HU; Mende, SB; Lu, G;

Published by: Published on:

YEAR: 2004 DOI:

Optical communications development for spacecraft applications

Bradley G. Boone, Jonathan R. Bruzzi, Bernard E. Kluga, Wesley P. Millard, Karl B. Fielhauer, Donald D. Duncan, Daniel V. Hahn, Christian W. Drabenstadt, Donald E. Maurer, and

Boone, Bradley; Bruzzi, Jonathan; Kluga, Bernard; Millard, Wesley; Fielhauer, Karl; Duncan, Donald; Hahn, Daniel; Drabenstadt, Christian; Maurer, Donald; Bokulic, Robert;

Published by: Johns Hopkins APL technical digest Published on:

YEAR: 2004 DOI:

First Three Years of TIMED: New Results in Sun-Earth Connections

Kozyra, JU; Crowley, G; Goncharenko, LP; Hagan, ME; Lu, G; Mlynczak, MG; Paxton, LJ; RUSSELL, JM; Solomon, SC; Talaat, ER; , others;

Published by: Published on:

YEAR: 2004 DOI:

Magnetotail behavior during storm time “sawtooth injections”

Lui, ATY; Hori, T; Ohtani, S; Zhang, Y; Zhou, XY; Henderson, MG; Mukai, T; Hayakawa, H; Mende, SB;

Published by: Journal of Geophysical Research: Space Physics Published on:

YEAR: 2004 DOI:

2003

TIMED ground system and Mission Operations

Elliot H. Rodberg, William P. Knopf, Paul M. Lafferty, and Stuart R. Nylund he Thermosphere, Ionosphere, Mesosphere Energetics and Dynamics (TIMED) mission operations concept

Rodberg, Elliot; Knopf, William; Lafferty, Paul; Nylund, Stuart;

Published by: Johns Hopkins APL technical digest Published on:

YEAR: 2003 DOI:

SA52A-0395

Galand, Marina; Lummzheim, Dirk; Frey, HU; Paxton, LJ; Christensen, AB;

Published by: Published on:

YEAR: 2003 DOI:

Comparison of the Modeled 135.6 nm Auroral Emission to TIMED GUVI Observations: Mapping Thermospheric Composition Variations During Auroral Events Above Alaska and Northwest Canada

Krynicki, MP; Conde, M; Lummerzheim, D; Paxton, L; Ishii, M;

Published by: Published on:

YEAR: 2003 DOI:

Storm-time ion pressure distribution of the inner magnetosphere