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The National Aeronautics and Space Administration (NASA) Global-scale Observations of the Limb and Disk (GOLD) satellite takes far-ultraviolet images of the Earth from geostationary orbit. GOLD observes the complete structure of equatorial plasma bubbles (EPBs). Since there are repeated observations of the same regions of the Earth, the zonal drift velocities of EPBs are derived using GOLD data. EPBs observed within 60-25°W longitudes on 27-29 November 2018 are considered in the present analysis. The drift velocities obtained on 27 November 2018 are 116 ± 4, 118 ± 6, and 105 ± 9 m/s at the North and South crests of equatorial ionization anomaly (EIA) and the magnetic equator, respectively. While on 29 November the velocities 107 ± 10, 106 ± 8, and 110 ± 4 m/s are in agreement with the 27th (within the uncertainties), on 28 November the velocities are substantially lower: 80 ± 3, 95 ± 7, and 88 ± 11 m/s. This is the first simultaneous measurement of EPB zonal drift velocities at both crests of EIA and the magnetic equator. On 27-29 November 2018, the average spacing between adjacent EPBs is found to be ~377, 526, and 442 km, respectively. [ABSTRACT FROM AUTHOR]

We report three different types of relativistic electron precipitation (REP) events observed at International Space Station (ISS), associated with electromagnetic ion cyclotron (EMIC) waves or whistler mode waves as observed by the Arase satellite at conjugate locations near the magnetic equator. Three different detectors installed on the ISS were complementarily used; CALET/CHD as the detector of precipitating MeV electrons, MAXI/RBM as the detector of sub-MeV electrons from horizontal and vertical directions, and SEDA-AP/SDOM to quantitatively measure the energy spectrum. The REP event on 21 August 2017 shows a quasiperiodic intensity variation at ~1 Hz which corresponds to variations of the EMIC waves at the Arase altitudes. The REP event on 24 April 2017 shows rapid and irregular intensity variation which corresponds to the amplitude variation of chorus waves, while the REP events on 26 October 2017 shows a smooth quasiperiodic time variation at ~0.2 Hz which corresponds to the amplitude variation of "electrostatic" whistler mode waves. This study clearly demonstrates that the time variation of REP events at ISS are caused by various types of plasma waves near the magnetic equator. [ABSTRACT FROM AUTHOR]

Based on the recalibrated data of >16-MeV proton omnidirectional integral fluxes obtained from NOAA POES and EUMETSAT MetOp satellites during the period from 1978 to 2014, solar cycle phase lags, the variations of proton radiation belt, and the relationships between trapped proton fluxes and F10.7 flux, cosmic ray, or sunspot number are investigated in detail. It is found that (a) the solar cycle phase lags between energetic proton fluxes and sunspot number are within 2.5 years, dependent on solar cycle, Lm, B/B0, and proton energy; (b) at the magnetic equator, the ratios of the maximal to minimal values of 4-month smoothed monthly >16-MeV proton fluxes during the period from 1978 to 2014 increase and then decrease with increasing Lm, showing the maximal value ~11.24 at Lm 1.15; and (c) at a magnetic field line with Lm = 1.15, the ratios of the maximal values in 1987 to the minimal values in 2002 for yearly >16-MeV proton fluxes decrease with increasing B/B0, while at a magnetic field line with Lm = 1.16, they increase and then decrease with increasing B/B0, and the maximal ratio for all magnetic field lines can reach above 20. An exponential equation with an offset is feasible to describe the relationship between the logarithm of >16-MeV proton fluxes and F10.7 flux. It can be readily used to improve the NOAAPRO model. [ABSTRACT FROM AUTHOR]

Whistler mode chorus waves in the Earth's inner magnetosphere are usually composed of discrete elements, and each element can be characterized by the following properties: the amplitude, the duration, the frequency span, and the frequency chirping rate. Using a one‐dimensional (1‐D) particle‐in‐cell (PIC) simulation code, we study the dependence of these properties of a rising‐tone chorus on the number density nheq/nc0 and temperature anisotropy AT of energetic electrons at the magnetic equator. The whistler waves are first excited around the magnetic equator by anisotropic energetic electrons and then develop into a rising‐tone chorus when they leave away from the equator. During the propagation toward the pole, the rising‐tone chorus with nearly constant frequency span first enhances and then decays. Its frequency chirping rate declines in the early stage and then gradually increases. Meanwhile, the chorus duration is quite the opposite due to propagation effect. Over a suitable range of nheq/nc0 to generate rising‐tone chorus, the frequency chirping rate of the excited rising‐tone chorus first increases and then saturates, while its saturated amplitude, duration, and frequency span have a rising tendency with the increasing nheq/nc0. As for AT, the frequency chirping rate of the generated rising‐tone chorus is increasing with the increase of AT that is consistent with prediction of nonlinear theory, while the duration is just the opposite. Our simulation study can give a further understanding of the generation and propagation of rising‐tone chorus waves. Key Points: The frequency chirping rate and the duration of the rising‐tone chorus excited near the magnetic equator change due to propagation effectThe amplitude, duration and frequency span of the rising‐tone chorus increase with the increasing number density of energetic electronsThe frequency chirping rate increases with increasing temperature anisotropy of energetic electrons, while the duration is the opposite [ABSTRACT FROM AUTHOR]

Information about the altitudinal distribution of ionospheric electron density (Ne) in the African equatorial region is very scanty. Such information is vital in modeling of key ionospheric parameters and in solving problems associated with ionospheric effect on the applications that depend on space‐based positioning and navigation systems. For the first time in the region, the entire Ne profile estimated by IRI is evaluated with profile deduced from Digisonde measurements at Ilorin (geog. 8.50°N, 4.50°E; dip. −7.9°) during low solar activity condition. Results obtained indicate marked discrepancies between the two profiles with magnitudes revealing local time and altitudinal and seasonal trends. The largest discrepancies are found between the post‐sunset and sunrise hours regardless of the seasons. IRI underestimates the Ne around the F1 region and is most obvious in September equinox and December solstice with deviation up to −42%. Further, IRI overestimates the Ne around the F2 peak at daytime, mostly in solstices with maximum deviation of 26% at F2 peak. All the three IRI topside models generally underestimate Ne between ~F2 peak height and ~800 km in all seasons except in June solstice. Beyond 800 km, the Digisonde, IRI‐NeQuick, and IRI‐2001 Corr profiles tend to converge, whereas the IRI‐2001 profiles still show marked divergence from the Digisonde profile in all seasons. Overall, the IRI‐NeQuick gives the best topside representation at this station at daytime/nighttime. The comparative analysis of Digisonde‐TEC and GPS‐TEC suggests that the Digisonde alone may not give a reliable estimate of the nighttime topside altitudinal distribution of Ne at this location. Key Points: The largest Digisonde‐IRI Ne profile divergences are found between the post‐sunset and sunrise hours irrespective of the seasonsIRI‐CCIR underestimates the Ne around the F1 altitudes and is most noticeable in September equinox and December solsticeDigisonde‐TEC versus GPS‐TEC suggests that the Digisonde alone may not give a reliable estimate of nighttime topside Ne distribution [ABSTRACT FROM AUTHOR]

The total electron content (TEC) data from Global Ionosphere Maps are used to obtain the tidal modes through two‐dimensional Fourier transform in both universal time and LT (local time) frames. In the LT frame, a north‐south TEC asymmetry is observed along the longitude, where there is a large displacement of the geomagnetic equator from the geographic equator. The phases of tidal modes lead to a constructive or destructive interference of contributing tidal modes, producing different zonal waves and longitudinal peaked structures at different local time (tLT). The summation of all nonmigrating zonal waves in the low‐latitude region (geomagnetic latitude < 30°) produces a peaked structure with two to four major peaks at most local hours. The amplitude of this peaked structure in June solstice is smaller than those in other seasons. During solar maximum (minimum), the amplitude of peaked structure has a value ~20 (~12) TECu with two to four (one to three) peaks. The locations of peaked structures formed by the nonmigrating tides in 2006 (solar minimum) and in 2014 (solar maximum) are similar. The Weddell Sea Anomaly is found to have a density enhancement in the region from 135°E to 90°W and from 40°S to 80°S with an amplitude ~19.85 (~5.07) TECu during March equinox (December solstice) of solar maximum (minimum). Key Points: The tidal modes obtained from TEC map generate, through constructive/destructive interference, different zonal waves and peaked structuresA north‐south TEC asymmetry is observed at the longitude, where the geomagnetic equator is largely displaced from the geographic equatorThe Weddell Sea Anomaly can be clearly observed from the summation of only nonmigrating tides [ABSTRACT FROM AUTHOR]