326 citations · 4.6k across the 86 of their papers we have counts for
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A Modified Version of Taylor's Hypothesis for Solar Probe Plus Observations
Kristopher G. Klein, Jean C. Perez, Daniel Verscharen +2
The Solar Probe Plus (SPP) spacecraft will explore the near-Sun environment, reaching heliocentric distances less than . Near Earth, spacecraft measurements of fluctu…
Deceleration of Alpha Particles in the Solar Wind by Instabilities and the Rotational Force: Implications for Heating, Azimuthal Flow, and the Parker Spiral Magnetic Field
Daniel Verscharen, Benjamin D. G. Chandran, Sofiane Bourouaine +1
Protons and alpha particles in the fast solar wind are only weakly collisional and exhibit a number of non-equilibrium features, including relative drifts between particle species.…
Stochastic Acceleration of Electrons by Fast Magnetosonic Waves in Solar Flares: the Effects of Anisotropy in Velocity andWavenumber Space
Peera Pongkitiwanichakul, Benjamin D. G. Chandran
We develop a model for stochastic acceleration of electrons in solar flares. As in several previous models, the electrons are accelerated by turbulent fast magnetosonic waves ("fas…
Turbulent Dissipation Challenge -- Problem Description
Tulasi N Parashar, Chadi Salem, Robert Wicks +4
The goal of this document is to present a detailed description of the goals, simulation setup and diagnostics for the Turbulent Dissipation Challenge (arXiv:1303.0204) as discussed…
Magnetohydrodynamic Slow Mode with Drifting He: Implications for Coronal Seismology and the Solar Wind
Joseph V. Hollweg, Daniel Verscharen, Benjamin D. G. Chandran
The MHD slow mode wave has application to coronal seismology, MHD turbulence, and the solar wind where it can be produced by parametric instabilities. We consider analytically how…
Intermittency and Alignment in Strong RMHD Turbulence
Benjamin D. G. Chandran, Alexander A. Schekochihin, Alfred Mallet
We develop an analytic model of intermittent, three-dimensional, strong, reduced magnetohydrodynamic turbulence with zero cross helicity. We take the fluctuation amplitudes to have…