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Articles by Joseph E. Borovsky
Estimating the length scales of magnetic-field-line wandering in the solar wind at 1 AU: ACE–earth magnetic-connection events
Abstract Open heliospheric magnetic-field lines wander along the Parker-spiral direction, and the length scale of the wandering provides information about the parallel wavelength of solar wind turbulence and affects scatter-free transport of energetic charged particles in the solar wind.
The correlations of energetic electron fluxes in the Earth’s central plasma sheet with solar wind variables and geomagnetic indices
Abstract Correlations between the electron fluxes in the Earth’s central plasma sheet and various solar wind and magnetospheric parameters are studied. Higher-energy fluxes (above approximately 2 keV) are the focus of the analysis. Flux measurements are taken during 950 current-sheet crossings in the central plasma sheet using 3-s-resolution electron measurements from the THEMIS-B and THEMIS-C spacecraft in the solar minimum years 2007–2010.
A mechanism of the auroral substorm expansion onset: electric discharge in the double layer
1 Introduction A magnetospheric substorm is a transient process initiated on the nightside of the Earth in which a significant amount of energy derived from the solar wind-magnetosphere interaction is deposited in the auroral ionosphere and in the magnetosphere (Rostoker et al., 1980).
Editorial: Driving towards a more diverse space physics research community-perspectives, initiatives, strategies, and actions
This Research Topic welcomed papers on diversity, equity, and inclusion (DEI) in the international space physics community. Demographics of the space physics research community have been documented by the American Geophysical Union1 and the American Astronomical Society2, both finding the memberships in these societies are strongly dominated by white men.
Reconnection in a pinch
Introduction Magnetic reconnection is the focus of the Magnetospheric Multiscale Mission (MMS), launched in March 2015 to investigate a process that had been invoked and identified for decades as an important factor in the storage and release of energy in the solar atmosphere and the magnetospheres of planets (Burch et al., 2016).
Testing adiabatic models of energetic electron acceleration at dipolarization fronts
1 Introduction Dipolarization fronts (DFs) are characterized by rapid increases in the z-component of the magnetic field in the magnetotail (e.g., Russell and McPherron, 1973; Angelopoulos et al., 1992; Nakamura et al., 2002). As the name suggests, these fronts carry a more dipolar field than the surrounding stretched tail field. The dipolarization of the tail is associated with substorms (e.g., Baumjohann et al., 1999; Fu et al., 2020, and references therein).
Editorial: Magnetosphere and ionosphere response to the solar wind transients
The uninterrupted stream of charged particles and magnetic fields that make up the solar wind dominates the interplanetary space. The solar wind is known to be highly variable and complex, consisting of different structures that vary in their spatial and temporal scales. When these transient structures from the solar wind interact with the Earth’s magnetic field, they generate a range of dynamics within the magnetosphere-ionosphere system.
Nuclear data for space exploration
1 Introduction Nuclear data has a wide range of utilizations, both in basic research and in applied fields. Space exploration is one of the applications where nuclear data plays a critical role—primarily due to the harmful effects of the space radiation environment. While both the nuclear science and space communities have identified many of the relevant nuclear physics issues to enable safe space exploration, they have been working relatively independently to address them.
Next-decade needs for 3-D ionosphere imaging
1 Introduction Accurate specification and modeling of the 3-D spatial variation together with the temporal evolution of Earth’s ionosphere has always been a strong need but a challenging task for the space weather community, as the ionosphere is a highly complicated geospace environment that exhibits not only remarkable climatological variation but also significant weather disturbances.
Turbulent dipolarization regions in the Earth’s magnetotail: ion fluxes and magnetic field changes
1 Introduction One way to obtain information about the state of astrophysical plasma is by studying the radiation they emit and that we remotely observe. Therefore, it is of essential importance to understand the mechanisms that contribute to the generation of radiation.
Unsolved problems: Mesoscale polar cap flow channels’ structure, propagation, and effects on space weather disturbances
Larry R. Lyons1*, Yukitoshi Nishimura2, Jiang Liu1,3, Ying Zou4, William A.
Survey of reconnection signatures in auroral oval ion precipitation
1 Introduction Signatures of reconnection in low Earth orbit (LEO) have been reported near the poleward edge of the auroral oval on both the dayside and the nightside for some time now. On the dayside, low-energy cutoff (LEC) ion spectra are routinely observed on the newly open field lines of the cusp and mantle (Newell and Meng, 1995), and their production mechanism has been modeled (Onsager et al., 1993; Wing et al., 1996).
Radio emissions of auroral origin observable at ground level: outstanding problems
1 Introduction There are four broad classifications of radio emissions of terrestrial auroral origin observable at ground level in the VLF band and at higher frequencies: 1) auroral cyclotron harmonic emissions, narrowband and occurring at cyclotron harmonics; 2) auroral medium frequency burst, broadband at 1.3–5.0 MHz; 3) auroral hiss, broadband below 1.3 MHz; and 4) leaked auroral kilometric radiation at hundreds of kHz. There are sub-types of each of these.
Effects of the evolving early Moon and Earth magnetospheres
1 Introduction The prevailing model for the generation of our Moon is the giant impact hypothesis in which a differentiated Mars-sized proto-planet impacted the proto-Earth during the early formation of the Solar System (Cameron and Benz, 1991; Canup and Asphaug, 2001), with the resulting debris forming the Earth and the Moon. The formation of the Moon begins just outside the Roche limit of ∼2.9 Earth radii (RE).
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