Statistical characteristics of the polar ionospheric scale height around the peak height of F2 layer with observations of the ESR radar: Quiet days

Qiao, Zheng; Yuan, Zhigang; Qi, Feng; Huang, Shiyong; Li, Haimeng; Li, Huimin; Li, Ming; Wang, Dedong

doi:10.1007/s11431-014-5729-4

Cited by 4 publications

(3 citation statements)

References 20 publications

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“…Topside scale heights in different definitions have been retrieved from diverse observations. Topside Ne profiles obtained from measurements including incoherent scatter radars (Lei et al, ; Liu, Le, et al, ; Liu, Wan, et al, ; Qiao et al, , ), radio occultations (Liu et al, ; Ma et al, ; Potula et al, ; Prol et al, ; Stankov & Jakowski, ; Su et al, ; S.‐C. Wang et al, ; Wu et al, ; T.‐L.…”

Section: Introductionmentioning

confidence: 99%

α‐Chapman Scale Height: Longitudinal Variation and Global Modeling

Liu

Jiang

et al. 2019

JGR Space Physics

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Scale height measures the altitude gradient of the electron density profile and relates with the ionospheric chemistry and dynamics, while its longitudinal variation has not been fully investigated in both statistical analyses and empirical modelings. In this study, 11-year electron density profiles from Constellation Observing System for Meteorology, Ionosphere, and Climate radio occultations are collected to retrieve the α-Chapman scale height (Hm) from the lower topside ionospheric electron density profile (within 200-km altitudes above the peak height of F2 layer [hmF2]) by fitting α-Chapman function with a constant scale height. The Hm shows evident longitudinal variations at midlatitudes, and its zonal structure shows a consistency with that of hmF2 during daytime, which indicates neutral winds change the ionospheric height and shape at the same time. Further, a global modeling of Hm named 2PCAFourier-Hm is built based on a two-layer Principle Component Analysis combined with Fourier regression analysis of its coefficients under low and moderated solar activity. Longitudinal variation is considered in the Hm's modeling, along with the variations of local time, latitude, day of the year, and solar activity. Overall, the model well captures the temporal and spatial variations of Hm with a root-mean-square error of 2.25 km and a correlation coefficient of 0.97 with respect to the Constellation Observing System for Meteorology, Ionosphere, and Climate observations. Plain Language Summary Scale height is the logarithmic altitude gradient of the electron density profile and tightly relates with ionospheric dynamics, plasma thermal structure, and composition. However, longitudinal dependence of scale height has not been fully investigated especially at midlatitudes. Longitudinal variation is such that ionospheric parameters show evident zonal difference at the same local time. Moreover, nearly no empirical models of scale height include the longitude as a variable though Liu et al. (2008, https://doi.org/10.1029/2008JA013490) found equatorial scale height has evident wave-like longitudinal variation.In this study, more than 4,100,000 samples of α-Chapman scale height (Hm) were retrieved from 11-year electron density profiles of Constellation Observing System for Meteorology, Ionosphere, and Climate. We found the midlatitude Hm has evident longitudinal variation, and its zonal structure is tightly relates with neutral winds' dynamics during daytime. Moreover, a five-dimensional (latitude, local time, longitude, day of year, and solar activity) empirical model of Hm is built based on a two-layer Principle Component Analysis combined with Fourier regression analysis of its coefficients. An executable MATLAB live code of this model is also provided in the supporting information.

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Section: Introductionmentioning

confidence: 99%

α‐Chapman Scale Height: Longitudinal Variation and Global Modeling

Liu

Jiang

et al. 2019

JGR Space Physics

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“…Goodman and Ballard [2004] also observed the variation of MUF to be least during summer and greatest in the equinox and winter periods. During the polar summer, solar radiation prevails the entire time with a slight variation in the intensity due to the changing solar elevation angles [Zheng et al, 2014]. In Figures 3c and 3d, the observed values are lower between 01:00 and 12:00 UT, increasing up to around 18:00 UT and decreasing until 24:00 UT.…”

Section: Resultsmentioning

confidence: 90%

Comparison of observed and predicted MUF(3000)F2 in the polar cap region

et al. 2015

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The maximum usable frequency for a 3000 km range circuit (MUF(3000)F2), computed from ionosonde measurements at Resolute (74.75 Predictions and observations show diurnal and seasonal variations; however, the VOACAP and ICEPAC models fail to reproduce the diurnal variation trend observed in the measurements during the summer period. The performance of these models has been statistically analysed: REC533 gives a better performance in winter and equinox months, while VOACAP has a better performance for both equinox and summer months. ICEPAC shows poor performance during low solar activity.

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“…They also explored the correlations between Hm and foF2, hmF2 and the IRI lower thickness parameter B0. Based on the EIS-CAT Svalbard Radar (ESR) observations, Qiao et al [39] statistically studied the Hm at high latitudes. With observations of the ESR between 1997 and 2008, they analyzed the statistical characteristics of the polar Hm with local time, season, and solar activity under quiet geomagnetic conditions.…”

Section: Ionospheric Climatology and Structuresmentioning

confidence: 99%