A study of the ionogram derived effective scale height around the ionospheric &amp;lt;I&amp;gt;hm&amp;lt;/I&amp;gt;F2

Liu, Liuming; Wan, Weixing; Ning, Baiqi

doi:10.5194/angeo-24-851-2006

Cited by 50 publications

(62 citation statements)

References 30 publications

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“…Therefore, the Hm variation near the dip equator would be also affected by the vertical E×B velocity. Moreover, the r values in this study are larger than those in Liu et al (2006) and Zhang et al (2006). This suggests that dependence of Hm on hmF2 is more obvious near the dip equator than at low-latitudes.…”

Section: Correlations Of Hm With Fof2 Hmf2 and B0contrasting

confidence: 65%

“…These results near the dip equator are not the totally same as those observed at other latitudes. At low-latitude, Liu et al (2006) showed that a weak negative or poor correlation exists between Hm and foF2 at Wuhan (30.6 • N, 114.4 • E). The poor correlation was also found Zhang et al (2006) using data from the low-latitude station, Hainan (19.4 • N, 109.0 • E).…”

Section: Correlations Of Hm With Fof2 Hmf2 and B0mentioning

confidence: 95%

“…Then, Reinisch et al (2004) showed that the Hm can help to improve the model of topside profile in International Reference Ionosphere (IRI) (Bilitza, 2001). Recently, the diurnal, seasonal, and solar activity variations of Hm at Wuhan (30.6 • N, 114.4 • E) and the yearly variation of Hm of Wuhan and 12 other stations were investigated by Liu et al (2006). The diurnal and seasonal variations of Hm at Hainan (19.4 • N, 109.0 • E) and two European stations were studied by Zhang et al (2006) and Mosert et al (2007), respectively.…”

Section: Introductionmentioning

confidence: 99%

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Quiet-condition variations in the scale height at F2-layer peak at Jicamarca during solar minimum and maximum

Lee

Reinisch

2007

Ann. Geophys.

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Abstract. This study is the first attempt to examine the quiet-condition variations in scale height (Hm) near the F2-layer peak in the equatorial ionosphere. The data periods of Hm derived from the Jicamarca ionograms are JanuaryDecember 1996 and April 1999-March 2000. The results show that the greatest and smallest Hm values are generally at 11:00-12:00 LT and 04:00-05:00 LT, respectively. Additionally, the sunrise peak occurs at 06:00 LT only during solar minimum. The post-sunset peaks in the equinoctial and summer months are more obvious during solar maximum. The Hm difference between solar minimum and maximum are significant from afternoon to midnight. On the other hand, the Hm values during 07:00-10:00 LT for solar minimum are close to those for solar maximum. Furthermore, the correlation of Hm with the critical frequency (foF2) of F2-layer is generally low. In contrast, the correlation between Hm and the peak height (hmF2) of F2-layer is high. For Hm and the thickness parameter (B0) of F2-layer, the correlation between these two parameters is almost perfect.

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Section: Correlations Of Hm With Fof2 Hmf2 and B0contrasting

confidence: 65%

Section: Correlations Of Hm With Fof2 Hmf2 and B0mentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

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Quiet-condition variations in the scale height at F2-layer peak at Jicamarca during solar minimum and maximum

Lee

Reinisch

2007

Ann. Geophys.

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“…With measurements from incoherent scatter radar, digisonde, topside sounder, and radio occultation techniques, the plasma scale heights around the F peak and the topside ionosphere are found to become larger at higher solar activity (Kutiev et al, 2006;Lei et al, 2005;Liu et al, 2006aLiu et al, , 2007aStankov and Jakowski, 2006), which will also increase plasma density at the DMSP altitude as a key role by further decreasing the reduced height z in Eq. (1).…”

Section: Discussionmentioning

confidence: 99%

The dependence of plasma density in the topside ionosphere on the solar activity level

et al. 2007

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Abstract. In this paper, the ten-year (1996)(1997)(1998)(1999)(2000)(2001)(2002)(2003)(2004)(2005) total ion density N i measurements from the Defense Meteorological Satellite Program (DMSP) spacecraft in the morning and evening (09:30 and 21:30 LT) sectors have been analyzed to explore the dependence of plasma densities in the topside ionosphere at middle and low latitudes on the solar activity level. Results indicate that there is a strong solar activity dependence of DMSP N i at 848 km altitude, which has latitudinal and seasonal features. The plasma density in the topside ionosphere has an approximately linear dependence on daily F107 and a strongly nonlinear dependence on SEM/SOHO EUV, such that the change rate of N i becomes greater with increasing solar EUV. This is quite different from the dependence of N i near the F-Region peak (NmF2), at which the rate of change of NmF2 decreases with increasing solar EUV. The rate of change of N i at the DMSP altitude is greatest in the latitude range where N i is greatest during high solar activity. We suggest that this greater rate of change (or amplification effect) of N i at the DMSP altitude is mainly a consequence of the solar activity variations of the topside scale height. The changes in the height of the F-Region peak (hmF 2 ) and the density NmF2 play a secondary role.

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“…They found that H m over Millstone Hill is overestimated by the IRI2001 model (Bilitza, 2001) and the temporal variations of H m can be explained in terms of those in the slab thickness. Liu et al (2006) reported that a moderate positive correlation is found between H m and the F 2 layer peak height (h m F 2 ) and a strong correlation between the bottomside thickness parameter B 0 and H m . A common feature is found at 13 global stations; that is, the values of H m are highest in summer and lowest in winter during daytime.…”

Section: Introductionmentioning

confidence: 99%

Variations of topside ionospheric scale heights over Millstone Hill during the 30-day incoherent scatter radar experiment

et al. 2007

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Abstract.A 30-day incoherent scatter radar (ISR) experiment was conducted at Millstone Hill (288.5 • E, 42.6 • N) from 4 October to 4 November 2002. The altitude profiles of electron density N e , ion and electron temperature (T i and T e ), and line-of-sight velocity during this experiment were processed to deduce the topside plasma scale height H p , vertical scale height VSH, Chapman scale height H m , ion velocity, and the relative altitude gradient of plasma temperature (dT p /dh)/T p , as well as the F 2 layer electron density (N m F 2 ) and height (h m F 2 ). These data are analyzed to explore the variations of the ionosphere over Millstone Hill under geomagnetically quiet and disturbed conditions. Results show that ionospheric parameters generally follow their median behavior under geomagnetically quiet conditions, while the main feature of the scale heights, as well as other parameters, deviated significantly from their median behaviors under disturbed conditions. The enhanced variability of ionospheric scale heights during the storm-times suggests that the geomagnetic activity has a major impact on the behavior of ionospheric scale heights, as well as the shape of the topside electron density profiles. Over Millstone Hill, the diurnal behaviors of the median VSH and H m are very similar to each other and are not so tightly correlated with that of the plasma scale height H p or the plasma temperature. The present study confirms the sensitivity of the ionospheric scale heights over Millstone Hill to thermal structure and dynamics. The values of VSH/H p tend to decrease as (dT p /dh)/T p becomes larger or the dynamic processes become enhanced.

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A study of the ionogram derived effective scale height around the ionospheric <I>hm</I>F2

Cited by 50 publications

References 30 publications

Quiet-condition variations in the scale height at F2-layer peak at Jicamarca during solar minimum and maximum

Quiet-condition variations in the scale height at F2-layer peak at Jicamarca during solar minimum and maximum

The dependence of plasma density in the topside ionosphere on the solar activity level

Variations of topside ionospheric scale heights over Millstone Hill during the 30-day incoherent scatter radar experiment

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