Coronal dimmings and what they tell us about solar and stellar coronal mass ejections [0.03%]
日冕暗化现象及其对太阳和恒星日冕物质抛射的启示
Astrid M Veronig,Karin Dissauer,Bernhard Kliem et al.
Astrid M Veronig et al.
Coronal dimmings associated with coronal mass ejections (CMEs) from the Sun have gained much attention since the late 1990s when they were first observed in high-cadence imagery of the SOHO/EIT and Yohkoh/SXT instruments. They appear as loc...
Solar irradiance measurements [0.03%]
太阳辐照度观测
Greg Kopp
Greg Kopp
The Sun provides nearly all the energy powering the Earth's climate system, far exceeding all other energy sources combined. The incident radiant energy, the "total solar irradiance," has been measured by an uninterrupted series of temporal...
Aline A Vidotto
Aline A Vidotto
How has the solar wind evolved to reach what it is today? In this review, I discuss the long-term evolution of the solar wind, including the evolution of observed properties that are intimately linked to the solar wind: rotation, magnetism ...
Mihir Desai,Joe Giacalone
Mihir Desai
Solar energetic particles, or SEPs, from suprathermal (few keV) up to relativistic ( ∼ few GeV) energies are accelerated near the Sun in at least two ways: (1) by magnetic reconnection-driven processes during solar flares resulting in...
Coronal mass ejections and their sheath regions in interplanetary space [0.03%]
太阳冕洞爆发及其在行星际空间中的鞘区结构
Emilia Kilpua,Hannu E J Koskinen,Tuija I Pulkkinen
Emilia Kilpua
Interplanetary coronal mass ejections (ICMEs) are large-scale heliospheric transients that originate from the Sun. When an ICME is sufficiently faster than the preceding solar wind, a shock wave develops ahead of the ICME. The turbulent reg...
Allan Sacha Brun,Matthew K Browning
Allan Sacha Brun
The Sun and other stars are magnetic: magnetism pervades their interiors and affects their evolution in a variety of ways. In the Sun, both the fields themselves and their influence on other phenomena can be uncovered in exquisite detail, b...
Daniel Verscharen,Kristopher G Klein,Bennett A Maruca
Daniel Verscharen
The solar wind is a magnetized plasma and as such exhibits collective plasma behavior associated with its characteristic spatial and temporal scales. The characteristic length scales include the size of the heliosphere, the collisional mean...
Shin Toriumi,Haimin Wang
Shin Toriumi
Strong solar flares and coronal mass ejections, here defined not only as the bursts of electromagnetic radiation but as the entire process in which magnetic energy is released through magnetic reconnection and plasma instability, emanate fr...
Solar prominences: theory and models: Fleshing out the magnetic skeleton [0.03%]
太阳日珥：理论与模型——磁骨架的构建与发展
Sarah E Gibson
Sarah E Gibson
Magnetic fields suspend the relatively cool material of solar prominences in an otherwise hot corona. A comprehensive understanding of solar prominences ultimately requires complex and dynamic models, constrained and validated by observatio...
Giulio Del Zanna,Helen E Mason
Giulio Del Zanna
X-ray and ultraviolet (UV) observations of the outer solar atmosphere have been used for many decades to measure the fundamental parameters of the solar plasma. This review focuses on the optically thin emission from the solar atmosphere, m...