scholarly journals Topside electron density profiles observed at low latitudes by COSMIC and compared with in situ ion densities measured by C/NOFS

2013 ◽  
Vol 118 (5) ◽  
pp. 2670-2680 ◽  
Author(s):  
Pei-Chen Lai ◽  
William J. Burke ◽  
L. C. Gentile
Keyword(s):  
Electron Density ◽  
Density Profiles ◽  
Low Latitudes ◽  
Electron Density Profiles

scholarly journals Deviations from model predictions in measured electron density profiles for low latitudes: A critique

2004 ◽  
Vol 43 (2) ◽  
pp. 165-172
Author(s):  
P. Muralikrishna ◽  
L. P. Vieira ◽  
M. A. Abdu ◽  
E. R. De Paula
Keyword(s):  
Electron Density ◽  
Density Profiles ◽  
Model Predictions ◽  
Low Latitudes ◽  
Electron Density Profiles

Se comparan los perfiles obtenidos in situ de las estaciones ecuatoriales de Brasil, usando pruebas de Langmuir y de Frecuencia de Alta Capacitancia, con las predicciones del modelo IRI, en el contexto de las distribuciones espectrales de las irregularidades observadas en la densidad del plasma. Se asume que las inestabilidades de Rayleigh-Taylor y la de Campo Cruzado, son las responsables de la generación de las irregularidades observadas en el plasma, y con ellas se estima el tiempo de crecimiento y el tamaño mínimo de las irregularidades que se observan en diferentes alturas para el perfil de densidad electrónica. Para ello se usan aproximaciones polinomiales simples para representar el perfil observado. La comparación entre las características de las irregularidades observadas del plasma con las esperadas a partir de la teoría nos puede dar información sobre la confiabilidad del perfil observado. La confiabilidad se vuelve particularmente importante de estimar debido a que las técnicas de medición de densidad electrónica se asocian a algunos problemas. Entonces se puede ver que si las desviaciones observadas del perfil comparadas con el modelo IRI son reales o no. De este estudio comparativo uno puede saber cuáles son los parámetros físicos responsables por las desviaciones observadas y sugerir mejoras en los métodos usados en las predicciones de IRI a bajas latitudes.

Mars’ ionopause characterization based on MAVEN and Mars Express observations

2020 ◽  
Author(s):  
Beatriz Sanchez-Cano ◽  
Clara Narvaez ◽  
Mark Lester ◽  
Michael Mendillo ◽  
Majd Mayyasi ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Magnetic Fields ◽  
Electron Density ◽  
Dynamic Pressure ◽  
Solar Wind Dynamic Pressure ◽  
Thermal Pressure ◽  
Density Profiles ◽  
Electron Density Profiles

<p>The ionopause is a tangential discontinuity in the ionospheric thermal plasma density profile that marks the upper boundary of the ionosphere for unmagnetized planets. Since only Venus and Mars have no global “dipole” magnetic fields, ionopauses are unique to those planets. For Venus, the ionopause formation is well characterized because the thermal pressure of the ionosphere is usually larger than the solar wind dynamic pressure. For Mars, however, the maximum thermal pressure of the ionosphere is usually insufficient to balance the total pressure in the overlying magnetic pileup boundary. Therefore, the Martian ionopause is not always formed, and when it does, it is highly structured and is located at different altitudes. In this study, we characterise the Martian ionopause formation from the point of view of the electron density and electron temperature, as well as the thermal, magnetic and dynamic pressures. The objective is to investigate under which circumstances the Martian ionopause is formed, both over and far from crustal magnetic fields, and compare to the Venus’ case. We use several multi-plasma and magnetic field in-situ observations from the three deep dip campaigns of the MAVEN mission that occurred on the dayside of Mars (near subsolar point), as well as in-situ solar wind plasma observations from the Mars Express mission. We find that that 36% of the electron density profiles over strong crustal magnetic field regions had an ionopause event in contrast to the 54% of electron density profiles far from strong crustal magnetic field regions. We also find that the topside ionosphere is typically magnetized at mostly all altitudes. The ionopause, if formed, occurs where the total ionospheric pressure (magnetic+thermal) equals the upstream solar wind dynamic pressure.</p>

Determination Of Daytime Midlatitude Electron Density Profiles From Satellite UV And In-Situ Data

1988 ◽  
Author(s):  
D. T. Decker ◽  
J. M. Retterer ◽  
J. R. Jasperse ◽  
D. N. Anderson ◽  
R. W. Eastes ◽  
...  
Keyword(s):  
Electron Density ◽  
Density Profiles ◽  
In Situ Data ◽  
Electron Density Profiles

On the deviations of measured electron density profiles from IRI predictions for low latitudes

2003 ◽  
Vol 31 (3) ◽  
pp. 563-568 ◽  
Author(s):  
P. Muralikrishna ◽  
L.P. Vieira ◽  
M.A. Abdu ◽  
E.R. de Paula
Keyword(s):  
Electron Density ◽  
Density Profiles ◽  
Low Latitudes ◽  
Electron Density Profiles

Electron density profiles above the F-layer

1973 ◽  
Vol 21 (9) ◽  
pp. 1581-1586
Author(s):  
Michael Anastassiadis ◽  
Georges Moraitis ◽  
Dimitris Matsoukas
Keyword(s):  
Electron Density ◽  
Density Profiles ◽  
Electron Density Profiles

scholarly journals Ionospheric assimilation techniques for ARGOS Low-Resolution Airglow and Aurora Spectrograph (LORAAS) tomographically reconstructed equatorial electron density profiles

Radio Science ◽  
2004 ◽  
Vol 39 (1) ◽  
pp. n/a-n/a ◽  
Author(s):  
J. J. Sojka ◽  
J. V. Eccles ◽  
R. W. Schunk ◽  
S. McDonald ◽  
S. Thonnard ◽  
...  
Keyword(s):  
Electron Density ◽  
Low Resolution ◽  
Density Profiles ◽  
Electron Density Profiles
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