What magnetospheric and ionospheric researchers should know about the solar wind

Borovsky, Joseph E.

doi:10.1016/j.jastp.2020.105271

Cited by 40 publications

(34 citation statements)

References 220 publications

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“…It should be mentioned that there are other factors beyond the shock impact angle that may affect the ULF wave response. For example, magnetospheric preconditions determined by preshock solar wind dynamic pressure and IMF B z may affect the subsequent magnetic activity (e.g., Borovsky, 2020; Zhou & Tsurutani, 2001). As another example, the magnetopause location prior to the shock arrival differs between the two events (Figure 2), and this could potentially affect frequency, amplitude, and spatial distribution; unfortunately, it is not possible to determine how the magnetopause location ultimately affects the ULF wave response after the shock arrives because we do not know where the magnetopause is located during the dynamic period immediately following the shock arrival.…”

Section: Resultsmentioning

confidence: 99%

Interplanetary Shock Impact Angles Control Magnetospheric ULF Wave Activity: Wave Amplitude, Frequency, and Power Spectra

Oliveira

Hartinger

et al. 2020

Geophysical Research Letters

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We present the first clear observational connection between interplanetary shock impact angles and magnetospheric ultralow frequency (ULF) wave activity. We perform a comparative study of two solar wind shocks with relatively similar strengths, but one being nearly frontal and, the other, highly inclined. We utilize multipoint observations with magnetometers based in space and on the ground for comparisons. For satellites and ground stations occupying similar local time positions, we find that the ULF waves have larger amplitudes and tend to be more narrowband in the case of the nearly head-on impact, confirming previous simulation results. Additionally, we provide evidence that, due to their symmetric compression nature, nearly frontal shocks can excite only odd mode waves, while asymmetric compressions caused by inclined shocks can excite both odd and even mode waves. These results suggest that shock impact angles play crucial roles in mediating ULF wave-particle interactions in the inner magnetosphere. Plain Language Summary The interaction of solar perturbations with the Earth's magnetic field is of paramount importance in space weather investigations. The subsequent response is almost always characterized by magnetic field disturbances measured in space and on the ground, which in turn can modulate energetic particle populations that damage satellite electronics and cause electric current surges in large-scale power transmission lines. These disturbances are also manifested as geomagnetic pulsations which in part are responsible for the distribution of energy in the near-Earth space environment. In this work, we connect, for the first time, observational properties of these pulsations or waves with the impact angle of the perturbation. We find that nearly head-on impacts are associated with stronger wave response in comparison to inclined impacts. These results show that space weather forecasters should take the perturbation impact angle into account when predicting geomagnetic effects caused by solar perturbations.

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Section: Resultsmentioning

confidence: 99%

Interplanetary Shock Impact Angles Control Magnetospheric ULF Wave Activity: Wave Amplitude, Frequency, and Power Spectra

Oliveira

Hartinger

et al. 2020

Geophysical Research Letters

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“…The mesoscale structure of the solar wind is also an important part of the Sun-Earth connection (Borovsky, 2020c). The temporal changes in the magnetic field associated with the passage of flux tubes results in sudden changes in the rate of dayside reconnection and the driving of the magnetosphere: Depending primarily on the local orientation of each tube, some flux tubes are geoeffective, some are not.…”

Section: Question 5: What Is the Origin And Evolution Of The Mesoscalmentioning

confidence: 99%

Nine Outstanding Questions of Solar Wind Physics

2020

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In situ measurements of the solar wind have been available for almost 60 years, and in that time plasma physics simulation capabilities have commenced and ground‐based solar observations have expanded into space‐based solar observations. These observations and simulations have yielded an increasingly improved knowledge of fundamental physics and have delivered a remarkable understanding of the solar wind and its complexity. Yet there are longstanding major unsolved questions. Synthesizing inputs from the solar wind research community, nine outstanding questions of solar wind physics are developed and discussed in this commentary. These involve questions about the formation of the solar wind, about the inherent properties of the solar wind (and what the properties say about its formation), and about the evolution of the solar wind. The questions focus on (1) origin locations on the Sun, (2) plasma release, (3) acceleration, (4) heavy‐ion abundances and charge states, (5) magnetic structure, (6) Alfven waves, (7) turbulence, (8) distribution‐function evolution, and (9) energetic‐particle transport. On these nine questions we offer suggestions for future progress, forward looking on what is likely to be accomplished in near future with data from Parker Solar Probe, from Solar Orbiter, from the Daniel K. Inouye Solar Telescope (DKIST), and from Polarimeter to Unify the Corona and Heliosphere (PUNCH). Calls are made for improved measurements, for higher‐resolution simulations, and for advances in plasma physics theory.

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“…Moreover, looking at Figure 1b, it is clear that the solar wind and selected geomagnetic activity indices data reveal correspondence Add solar wind and geomagnetic activity data time histories. In step (b) we aligned the instantaneous features (solar wind and geomagnetic activity indices) to the DMSP observation data samples, but recognize that previous information from the solar wind and ionosphere and magnetosphere are also important to current particle precipitation and substorm behavior (Borovsky, 2020b, and references therein). In order to capture such information, we attach to the data samples the time histories of each of the solar wind and geomagnetic activity indices data.…”

Section: The Heliophysics and Space Weather Data Landscape In The Context Of Particle Precipitationmentioning

confidence: 99%

Toward a Next Generation Particle Precipitation Model: Mesoscale Prediction Through Machine Learning (a Case Study and Framework for Progress)

et al. 2021

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Electron precipitation is a key component linking the ionosphere and the magnetosphere. Electrons in the magnetosphere-ionosphere (MI) system carry current, transport energy, and precipitate (i.e., follow magnetic field lines from the magnetosphere to the ionosphere) to collide with the neutral atmosphere thereby driving changes in the electrical conductivity tensor. This tensor is central to the three-dimensional electrical current circuit that flows over vast distances between the magnetosphere and the ionosphere. Indeed, particle precipitation is a key input to all global circulation models (GCMs) such as the Global Ionosphere Thermosphere Model (GITM) (Ridley et al., 2006), the Thermosphere Ionosphere Electrodynamics General Circulation Model (TIE-GCM) (Roble et al., 1988), and the Whole Atmosphere Model-Ionosphere

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What magnetospheric and ionospheric researchers should know about the solar wind

Cited by 40 publications

References 220 publications

Interplanetary Shock Impact Angles Control Magnetospheric ULF Wave Activity: Wave Amplitude, Frequency, and Power Spectra

Interplanetary Shock Impact Angles Control Magnetospheric ULF Wave Activity: Wave Amplitude, Frequency, and Power Spectra

Nine Outstanding Questions of Solar Wind Physics

Toward a Next Generation Particle Precipitation Model: Mesoscale Prediction Through Machine Learning (a Case Study and Framework for Progress)

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