ISS FPP Ionospheric Electron Density and Temperature Measurements - Results, Comparison with the IRI-90 Model, and Implications for ISS Charging

Author(s):  
Dale Ferguson ◽  
Thomas Morton ◽  
G. Hillard ◽  
Robert Personen
2011 ◽  
Vol 415 (1) ◽  
pp. S1166-S1169
Author(s):  
R. Laengner ◽  
B. Unterberg ◽  
A. Lyssoivan ◽  
M. Paul ◽  
V. Philipps ◽  
...  

2008 ◽  
Vol 680 (2) ◽  
pp. 1477-1495 ◽  
Author(s):  
Markus J. Aschwanden ◽  
Nariaki V. Nitta ◽  
Jean‐Pierre Wuelser ◽  
James R. Lemen

1997 ◽  
Vol 82 (5) ◽  
pp. 2140-2146 ◽  
Author(s):  
S. S. Harilal ◽  
C. V. Bindhu ◽  
Riju C. Issac ◽  
V. P. N. Nampoori ◽  
C. P. G. Vallabhan

2018 ◽  
Vol 36 (3) ◽  
pp. 855-866
Author(s):  
Moran Liu ◽  
Chen Zhou ◽  
Xiang Wang ◽  
Bin Bin Ni ◽  
Zhengyu Zhao

<p><strong>Abstract.</strong> In this paper, we investigate the ionospheric heating by oblique incidence of powerful high-frequency (HF) radio waves using three-dimensional numerical simulations. The ionospheric electron density and temperature perturbations are examined by incorporating the ionospheric electron transport equations and ray-tracing algorithm. The energy distribution of oblique incidence heating waves in the ionosphere is calculated by the three-dimensional ray-tracing algorithm. The calculation takes into consideration the electric field of heating waves in the caustic region by the plane wave spectral integral method. The simulation results show that the ionospheric electron density and temperature can be disturbed by oblique incidence of powerful radio waves, especially in the caustic region of heating waves. The oblique ionospheric heating with wave incidence parallel and perpendicular to the geomagnetic field in the mid-latitude ionosphere is explored by simulations, results of which indicate that the ionospheric modulation is more effective when the heating wave propagates along the magnetic field line. Ionospheric density and temperature striations in the caustic region due to thermal self-focusing instability are demonstrated, as well as the time evolution of the corresponding fluctuation spectra.</p>


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