2002
DOI: 10.1029/2001ja900142
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Possible hydrodynamic waves in the topside ionospheres of Mars and Venus

Abstract: The dispersion relation for hydrodynamic waves in an ionosphere with at most a weak magnetic field shows that gravity waves as well as hydrodynamic hybrid waves may be excited in the topside ionosphere of Mars and Venus owing to fluctuations in the solar wind pressure. The gravity wave, which propagates horizontally with a frequency equal to the buoyancy frequency, belongs to the classic branches of acoustic‐gravity wave (AGW) mode. The hybrid waves result from coupling between two different hydrodynamic wave … Show more

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Cited by 14 publications
(11 citation statements)
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“…These waves should always be present in the Martian daytime ionosphere, except when the solar wind pressure is very high. The same theory has been applied to Venus and results similar to Mars were predicted [ Wang and Nielsen , 2002a, 2002b]. Pioneer Venus Obiter radio occultation measurements also display fluctuations of the electron density [e.g., Kliore , 1992].…”
Section: Discussionmentioning
confidence: 95%
“…These waves should always be present in the Martian daytime ionosphere, except when the solar wind pressure is very high. The same theory has been applied to Venus and results similar to Mars were predicted [ Wang and Nielsen , 2002a, 2002b]. Pioneer Venus Obiter radio occultation measurements also display fluctuations of the electron density [e.g., Kliore , 1992].…”
Section: Discussionmentioning
confidence: 95%
“…The question is therefore to what degree waves may contribute to plasma acceleration and, if so, where the waves are generated and how they access the ionosphere. Wang and Nielsen (2002) reported on what they interpreted as hydrodynamic waves in the topside ionosphere of Mars, i.e. strong electron density modulations reaching down to some 200 km altitude.…”
Section: Plasma Acceleration By Wavesmentioning
confidence: 96%
“…Plasma waves have also been observed near Mars (e.g. Wang and Nielsen 2002;Espley et al 2004;Ergun et al 2006), but lacking simultaneous particle, field, and wave measurements we must rely on theory and a qualitative analysis. The relation between waves and the wavelike modulation of ions and electrons, was considered by Winningham et al (2006), Gunell et al (2008) and , the latter in an analysis of the auroral plasma acceleration above regions of crustal magnetic field at Mars.…”
Section: Plasma Acceleration By Wavesmentioning
confidence: 98%
“…This "80 hours rule", as the simplest prediction tool, seems to work well in many cases, especially near solar activity minimum. Wang, Ye and Wang (2002) studied 15 events that were associated with severe storms (K p > 7) and found that the transit time of the CMEs can be predicted by this formula T = 27.98 + 2.11 × 10 4 /V p where V p (km/s) is the CME projected speed and T (hours) is the transit time of the CME defined as the interval from CME's first appearance in C2 to to the beginning of the maximum K p index of the associated geomagnetic storm. Srivastava and Venkatakrishnan (2004) determined an empirical relation between the transit time and the initial speed from 64 CME events T = 86.9 − 0.026V p Here T (hours) is the difference in the timings of the start of the CME and the time of the onset of the geomagnetic storm marked by the decrease in Dst values, while V p (km/s) is also the CME projected speed.…”
Section: The Prediction Of Cme's Transit Timementioning
confidence: 97%
“…2 The frequency distribution of heliographic latitudes (a) and heliographic longitudes (b) of the CME sources. The event numbers are summed over 10 degree bins, and in (b) the longitude refers to longitudinal displacement from central meridian the results of related studies (Cane, Richardson and St. Cyr, 2000;Wang et al, 2002;Manoharan et al, 2004;Srivastava and Venkatakrishnan, 2004;Shrivastava and Singh, 2005). As a contrast, Fig.…”
Section: The Same Side-opposite Side Effect For Cmes and Their Geoeffmentioning
confidence: 98%