Multi-scale variability of coronal loops set by thermal non-equilibrium and instability as a probe for coronal heating
Solar coronal loops are the building blocks of the solar corona. These dynamic structures
are shaped by the magnetic field that expands into the solar atmosphere. They can be …
are shaped by the magnetic field that expands into the solar atmosphere. They can be …
Magnetohydrodynamic waves in open coronal structures
D Banerjee, S Krishna Prasad, V Pant… - Space Science …, 2021 - Springer
Modern observatories have revealed the ubiquitous presence of magnetohydrodynamic
waves in the solar corona. The propagating waves (in contrast to the standing waves) are …
waves in the solar corona. The propagating waves (in contrast to the standing waves) are …
Shear-driven transition to isotropically turbulent solar wind outside the Alfvén critical zone
Shear-driven Transition to Isotropically Turbulent Solar Wind Outside the Alfvén Critical Zone -
IOPscience This site uses cookies. By continuing to use this site you agree to our use of …
IOPscience This site uses cookies. By continuing to use this site you agree to our use of …
Nine outstanding questions of solar wind physics
NM Viall, JE Borovsky - Journal of Geophysical Research …, 2020 - Wiley Online Library
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 …
time plasma physics simulation capabilities have commenced and ground‐based solar …
Transient small-scale brightenings in the quiet solar corona: A model for campfires observed with Solar Orbiter
Context. Recent observations by the Extreme Ultraviolet Imager (EUI) on board Solar Orbiter
have characterized prevalent small-scale transient brightenings in the corona above the …
have characterized prevalent small-scale transient brightenings in the corona above the …
Ultra-high-resolution observations of persistent null-point reconnection in the solar corona
Magnetic reconnection is a key mechanism involved in solar eruptions and is also a prime
possibility to heat the low corona to millions of degrees. Here, we present ultra-high …
possibility to heat the low corona to millions of degrees. Here, we present ultra-high …
Turbulent magnetic reconnection generated by intense lasers
Y Ping, J Zhong, X Wang, B Han, W Sun, Y Zhang… - Nature Physics, 2023 - nature.com
Turbulent magnetic reconnection is believed to occur in astrophysical plasmas, and it has
been suggested to be a trigger of solar flares. It often occurs in long stretched and …
been suggested to be a trigger of solar flares. It often occurs in long stretched and …
Quasi-periodic energy release and jets at the base of solar coronal plumes
Coronal plumes are long, ray-like, open structures that have been considered as possible
sources of the solar wind. Their origin in the largely unipolar coronal holes has long been a …
sources of the solar wind. Their origin in the largely unipolar coronal holes has long been a …
Mapping the magnetic field in the solar corona through magnetoseismology
Magnetoseismology, a technique of magnetic field diagnostics based on observations of
magnetohydrodynamic (MHD) waves, has been widely used to estimate the field strengths …
magnetohydrodynamic (MHD) waves, has been widely used to estimate the field strengths …
A comprehensive radiative magnetohydrodynamics simulation of active region scale flux emergence from the convection zone to the corona
F Chen, M Rempel, Y Fan - The Astrophysical Journal, 2022 - iopscience.iop.org
We present a comprehensive radiative magnetohydrodynamic simulation of the quiet Sun
and large solar active regions. The 197 Mm wide simulation domain spans from 18 (10) Mm …
and large solar active regions. The 197 Mm wide simulation domain spans from 18 (10) Mm …