A Comparative Study on the Factors Controlling the Cusp Auroral Intensity Between the Northern and Southern Hemispheres

Qiu, Hui‐Xuan; Han, Desheng; Zhang, Hong‐Da; Yang, Huigen; Feng, Hui‐Ting; Yu, Xin; Shi, Run; Zhou, Su; Zhang, Yongliang

doi:10.1029/2021ja030216

Cited by 1 publication

(1 citation statement)

References 47 publications

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“…11a and 13a). It has been shown that the B y component of the IMF can lead to interhemispheric asymmetries in the intensity of the aurora not only on the dayside (Qiu et al, 2022), but also on the nightside (Liou & Mitchell, 2019). Therefore, future work could explore to what extent these asymmetries can be found in auroral proton precipitation obtained with Vlasiator, should a 3D-3V run with a nonzero IMF B y become available.…”

Section: Limitations Of the Current Setupmentioning

confidence: 99%

First 3D hybrid-Vlasov global simulation of auroral proton precipitation and comparison with satellite observations

Grandin¹,

Luttikhuis²,

Battarbee³

et al. 2023

J. Space Weather Space Clim.

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The precipitation of charged particles from the magnetosphere into the ionosphere is one of the crucial coupling mechanisms between these two regions of geospace and is associated with multiple space weather effects, such as global navigation satellite system signal disruption and geomagnetically induced currents at ground level. While precipitating particle fluxes have been measured by numerous spacecraft missions over the past decades, it often remains difficult to obtain global precipitation patterns with a good time resolution during a substorm. Numerical simulations can help to bridge this gap and improve the understanding of mechanisms leading to particle precipitation at high latitudes through the global view they offer on the near-Earth space system. We present the first results on auroral (0.5–50 keV) proton precipitation within a 3-dimensional simulation of the Vlasiator hybrid-Vlasov model. The run is driven by southward interplanetary magnetic field conditions with constant solar wind parameters. We find that, on the dayside, cusp proton precipitation exhibits the expected energy–latitude dispersion and takes place in the form of successive bursts associated with the transit of flux transfer events formed through dayside magnetopause reconnection. On the nightside, the precipitation takes place within the expected range of geomagnetic latitudes, and it appears clearly that the precipitating particle injection is taking place within a narrow magnetic local time span, associated with fast Earthward plasma flows in the near-Earth magnetotail. Finally, the simulated precipitating fluxes are compared to observations from Defense Meteorological Satellite Program spacecraft during driving conditions similar to those in the simulation and are found to be in good agreement with the measurements.

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Section: Limitations Of the Current Setupmentioning

confidence: 99%