Density Perturbations in the Upper Atmosphere Caused by the Dissipation of Solar Wind Energy

Prölss, Gerd W.

doi:10.1007/s10712-010-9104-0

Cited by 121 publications

(166 citation statements)

References 265 publications

(124 reference statements)

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“…3 mostra esquematicamente como a termosfera recebe energia solar [39]. A principal fonte de energia e momentum que entra no sistema ITé a radiação solar de comprimento de onda de 10-124 nm denominada radiação ultravioleta extrema (extreme ultraviolet, EUV, sigla em inglês).…”

Section: A Termosfera Durante Tempestades Geomagnéticasunclassified

“…Por exemFigura 3: Os principais modos de transmissão de energia solarà termosfera: radiação UV e aquecimento Joule. Figura extraída e adaptada da literatura [39].…”

Section: A Termosfera Durante Tempestades Geomagnéticasunclassified

“…Regiões de altas latitudes incluem as zonas aurorais e a calota polar [39]. As zonas aurorais são as regiões que recebem maior quantidade de energia eletromagnética durante tempestades geomagnéticas [53][54][55].…”

Section: A Termosfera Durante Tempestades Geomagnéticasunclassified

“…As zonas aurorais são as regiões que recebem maior quantidade de energia eletromagnética durante tempestades geomagnéticas [53][54][55]. Devido ao constante incremento de energia nessas regiões, estruturas de grande escala denominadas ondas de gravidade ou perturbações atmosféricas em movimento (TADs, do inglês traveling atmospheric disturbances) são lançadas a regiões de baixas latitudes [39,54,[56][57][58][59][60]. Regiões de altas latitudes da termosfera são aquecidas em minutos, mas a energia se globaliza em aproximadamente 3 horas [51].…”

Section: A Termosfera Durante Tempestades Geomagnéticasunclassified

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Reação da termosfera a tempestades geomagnéticas

Oliveira

Silveira

2017

Rev. Bras. Ensino Fís.

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A termosferaé uma das camadas mais externas da atmosfera terrestre, localizada entre 90-1000 km de altitude, logo abaixo da exosfera. Composta porátomos e moléculas neutras, ou partículas neutras, a termosferaé extremamente sensívelà variações de energia nela depositada. Durante a ocorrência de tempestades geomagéticas, moderadas ou intensas, uma grande quantidade de energia e momentum são depositadas em regiões de alta latitude da termosfera. O plasma, proveniente do vento solar,é energizado na magnetosfera e ao atingir a termosfera provoca o aquecimento das partículas neutras e a elevação da camada. As perturbações causadas pelas tempestades geomagnéticas na termosfera afetam asórbitas de satélites e outros objetos que transitam nessa região. Assim, o estudo de tais efeitosé extremamente importante do ponto de vista científico e tecnológico. Neste artigo, apresentaremos uma revisão das principais características da termosfera durante intervalos de calmaria (sem tempestades) e intervalos de tempestade. Logo após, discutiremos os efeitos provocados na termosfera pela tempestade geomagnética ocorrida em 20 de novembro de 2003. Para exemplificar os efeitos causados na termosfera, apresentaremos dados de densidade de partículas neutras observados pelo acelerômetro a bordo de um satélite de baixá orbita (LEO, do inglês low-Earth orbit) coletados durante aquela tempestade geomagnética. Palavras-chave: Tempestades geomagnéticas, interações MIT, elevação de partículas neutras na termosfera.The thermosphere is one of the highest layers of the Earth's atmosphere, localized in altitude regions between 90-1000 km, right below the exosphere. Composed of neutral atoms and molecules, or neutral particles, the thermosphere is extremely sensitive to variations of energy input. During the occurrence of moderate or intense geomagnetic storms, large quantities of plasma energy and momentum are deposited in high latitude regions of the thermosphere. Solar wind plasma, previously energized by the magnetosphere, reaches the thermosphere causing the heating and upwelling of neutral particles. The thermosphere disturbances caused by geomagnetic storms affect the orbit of satellites and other objects that fly in that region. Therefore, the study of such effects are extremely important in the scientific and technological view. In this paper, we present a review of the main characteristics of the thermosphere during quiet times (no storms) and during storm times. Then, we discuss the effects caused by the 20 November 2003 geomagnetic storm on the thermosphere. As an example, we present data of neutral density observed by the accelerometer onboard a LEO (low-Earth orbit) satellite during that geomagnetic storm.

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Section: A Termosfera Durante Tempestades Geomagnéticasunclassified

“…Por exemFigura 3: Os principais modos de transmissão de energia solarà termosfera: radiação UV e aquecimento Joule. Figura extraída e adaptada da literatura [39].…”

Section: A Termosfera Durante Tempestades Geomagnéticasunclassified

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Reação da termosfera a tempestades geomagnéticas

Oliveira

Silveira

2017

Rev. Bras. Ensino Fís.

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“…As a result of the combined impact, the ionospheric structure is substantially altered at global scale to compose a complex sequence of ionospheric disturbances. Among others, large-scale increases and decreases in the peak electron density, the so called positive and negative storm effects respectively that appear with strong seasonal, latitudinal and local time dependence hold a critical role (see for example the review articles presented by Rishbeth, 1991;Prölss, 1995;Buonsanto, 1999 andMendillo, 2006).…”

Section: Introductionmentioning

confidence: 99%

A new short-term forecasting model for the total electron content storm time disturbances

Tsagouri

Koutroumbas

Elias

2018

J. Space Weather Space Clim.

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-This paper aims to introduce a new model for the short-term forecast of the vertical Total Electron Content (vTEC). The basic idea of the proposed model lies on the concept of the Solar Wind driven autoregressive model for Ionospheric short-term Forecast (SWIF). In its original version, the model is operationally implemented in the DIAS system (http://dias.space.noa.gr) and provides alerts and warnings for upcoming ionospheric disturbances, as well as single site and regional forecasts of the foF2 critical frequency over Europe up to 24 h in advance. The forecasts are driven by the real time assessment of the solar wind conditions at ACE location. The comparative analysis of the variations in foF2 and vTEC during eleven geomagnetic storm events that occurred in the present solar cycle 24 reveals similarities but also differences in the storm-time response of the two characteristics with respect to the local time and the latitude of the observation point. Since the aforementioned dependences drive the storm-time forecasts of the SWIF model, the results obtained here support the upgrade of the SWIF's modeling technique in forecasting the storm-time vTEC variation from its onset to full development and recovery. According to the proposed approach, the vTEC storm-time response can be forecasted from 1 to 12-13 h before its onset, depending on the local time of the observation point at storm onset at L1. Preliminary results on the assessment of the performance of the proposed model and further considerations on its potential implementation in operational mode are also discussed.

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Altitude variations in the thermosphere mass density response to geomagnetic activity during the recent solar minimum

et al. 2014

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Accelerometer data from coplanar orbits of Challenging Minisatellite Payload (CHAMP) and Gravity Recovery and Climate Experiment (GRACE) satellites were used to study the complex altitude and latitude variations of the thermosphere mass density response to geomagnetic activity during 1-10 December 2008 near 09 LT. Helium number densities near 500 km altitude were extracted from the CHAMP and GRACE measurements and clearly show the presence of a winter hemisphere helium bulge. This recent extreme solar minimum indicates that wintertime helium concentrations exceed NRLMSISE-00 model estimates by 30%-70% during quiet geomagnetic activity after adjusting F 10.7 input into MSIS. The perturbation in mass density from quiet to active conditions is found to be less enhanced in the winter hemisphere at the higher GRACE altitudes (25%) than at the lower CHAMP altitudes (60%) and is attributed to dynamic behavior in the helium/oxygen transition. The investigation revealed the maximum storm time density perturbation to occur near the He/O transition region with a much weaker maximum near the O/N 2 transition region. The altitude of maximum density perturbation occurs where the perturbation in the weighted pressure scale height is equal and opposite to the perturbation in the weighted mean molecular weight scale height. The altitude structure of density scale height perturbation is significantly influenced by the changes in the molecular weight scale height and can account for 50% of the change in mass density scale height in a region correspondingly close to the He/O transition during the 2008 solar minimum period.

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Density Perturbations in the Upper Atmosphere Caused by the Dissipation of Solar Wind Energy

Cited by 121 publications

References 265 publications

Reação da termosfera a tempestades geomagnéticas

Reação da termosfera a tempestades geomagnéticas

A new short-term forecasting model for the total electron content storm time disturbances

Altitude variations in the thermosphere mass density response to geomagnetic activity during the recent solar minimum

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