Space Weather

doi:10.1002/9781118668351

Cited by 4 publications

(3 citation statements)

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“…Later, the statistical approach was employed by Chernogor and Domnin (2014). The statistics of magnetic and ionospheric storms are presented in Vijaya Lekshmi et al (2011), Yakovchouk et al (2012), and Zolotukhina et al (2018).…”

Section: Introductionmentioning

confidence: 99%

“…The results of recent studies of ionospheric storm effects are presented in a large number of papers (see, e.g., Blanch et al, 2005;Mendillo, 2006;Pirog et al, 2006;Prölss, 2006;Kamide and Maltsev, 2007;Borries et al, 2015;Liu et al, 2016;Polekh et al, 2017;Shpynev et al, 2018;Yamauchi et al, 2018;Blagoveshchensky and Sergeeva, 2019;Chernogor et al, 2020;Mosna et al, 2020).…”

Section: Introductionmentioning

confidence: 99%

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Dynamic processes in the magnetic field and in the ionosphere during the 30 August–2 September 2019 geospace storm: influence on high frequency radio wave characteristics

et al. 2021

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Abstract. The concept that geospace storms are comprised of synergistically coupled magnetic storms, ionospheric storms, atmospheric storms, and storms in the electric field originating in the magnetosphere, the ionosphere, and the atmosphere (i.e., electrical storms) was validated a few decades ago. Geospace storm studies require the employment of multiple-method approaches to the Sun–interplanetary medium–magnetosphere–ionosphere–atmosphere–Earth system. This study provides general analysis of the 30 August–2 September 2019 geospace storm, the analysis of disturbances in the geomagnetic field and in the ionosphere, as well as the influence of the ionospheric storm on the characteristics of high frequency (HF) radio waves over the People's Republic of China. The main results of the study are as follows. The energy and power of the geospace storm have been estimated to be 1.5×1015 J and 1.5×1010 W, and thus, this storm is weak. The energy and power of the magnetic storm have been estimated to be 1.5×1015 J and 9×109 W, i.e., this storm is moderate, and a characteristic feature of this storm is the duration of the main phase of up to 2 d. The recovery phase also was lengthy and was no less than 2 d. On 31 August and 1 September 2019, the variations in the H and D components attained 60–70 nT, while the Z-component variations did not exceed 20 nT. On 31 August and 1 September 2019, the level of fluctuations in the geomagnetic field in the 100–1000 s period range increased from 0.2–0.3 to 2–4 nT, while the energy of the oscillations showed a maximum in the 300–400 to 700–900 s period range. During the geospace storm, a moderately to strongly negative ionospheric storm manifested itself by the reduction in the ionospheric F-region electron density by a factor of 1.4 to 2.4 times on 31 August and 1 September 2019, compared to the its values on the reference day. Appreciable disturbances were also observed to occur in the ionospheric E region and possibly in the Es layer. In the course of the ionospheric storm, the altitude of reflection of radio waves could sharply increase from ∼150 to ∼300–310 km. The atmospheric gravity waves generated within the geospace storm modulated the ionospheric electron density; for the ∼30 min period oscillation, the amplitude of the electron density disturbances could attain ∼40 %, while it did not exceed 6 % for the ∼15 min period. At the same time, the height of reflection of the radio waves varied quasi-periodically with a 20–30 km amplitude. The results obtained have made a contribution to the understanding of the geospace storm physics, to developing theoretical and empirical models of geospace storms, to the acquisition of detailed understanding of the adverse effects that geospace storms have on radio wave propagation, and to applying that knowledge to effective forecasting of these adverse influences.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Dynamic processes in the magnetic field and in the ionosphere during the 30 August–2 September 2019 geospace storm: influence on high frequency radio wave characteristics

et al. 2021

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The VLF Transmitter, Narrowband Receiver, and Tuner Investigation on the DSX Spacecraft

et al. 2023

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Background and MotivationUnderstanding, specification, and mitigation of the geomagnetically trapped radiation effects on human activity in space have been topics of intense interest since the discovery of the Van Allen belts in 1958, for example, Song et al. (2001). Concerns about damage to Earth-orbiting satellite systems and humans in space have led to studies of ways such threats may be mitigated through controlled precipitation of energetic electrons from the radiation belts (Kennel & Petschek, 1966). Loss of energetic electrons from the radiation belts is known to occur as a result of Doppler-shifted gyro-resonance interactions with in situ VLF, or physically, whistler-mode waves, examples being scattering by lightning-generated whistlers, magnetospheric activity-related whistler-triggered wave bursts, bursts of natural whistler-mode noise, and whistler-mode signals from high-power ground-based VLF communication transmitters (Abel & Thorne, 1998;Imhof et al., 1983). Here we note that the whistler mode may cover

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Ionospheric storm effects over the People’s Republic of China on 14 May 2019: Results from multipath multi-frequency oblique radio sounding

Черногор

Гармаш

Guo

et al. 2020

Advances in Space Research

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Space Weather

Cited by 4 publications

References 342 publications

Dynamic processes in the magnetic field and in the ionosphere during the 30 August–2 September 2019 geospace storm: influence on high frequency radio wave characteristics

Dynamic processes in the magnetic field and in the ionosphere during the 30 August–2 September 2019 geospace storm: influence on high frequency radio wave characteristics

The VLF Transmitter, Narrowband Receiver, and Tuner Investigation on the DSX Spacecraft

Ionospheric storm effects over the People’s Republic of China on 14 May 2019: Results from multipath multi-frequency oblique radio sounding

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