Titlebook: Eruptions on the Sun; Boris Filippov Book 2024 The Editor(s) (if applicable) and The Author(s), under exclusive license to Springer Nature

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General Characteristics of the Sun,cribed. More attention is paid to the solar atmosphere, where solar activity phenomena are rape and developed. Some instruments for observations of the Sun, especially the upper layers of the solar atmosphere, which are impossible from the ground level, are listed, as well as space missions dedicate

警告

Magnetic Fields on the Sun,itting of spectral lines in the early twentieth century. After the invention of the photoelectric solar magnetograph in the mid-twentieth century, it became clear that magnetic fields are present almost everywhere in the photosphere, but they are distributed very unevenly. The strongest fields are o

妨碍议事

Equilibrium Plasma Structures in the Solar Atmosphere,magnetic field for a long time. Solar prominences were discovered long ago during total eclipse observations. Their types, properties, and magnetic structure are described. The location of prominences on the solar disk and their internal fine structure suggest that prominence plasma is supported and

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Intimate Relationship Between Plasma Structures and Magnetic Fields in the Solar Atmosphere,on and internal structure of coronal plasma formations. Prominences are elongated along large-scale polarity inversion lines of the photospheric magnetic field (neutral lines). It is shown that the prominence material is concentrated close to the magnetic neutral surface or the surface passing throu

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Peculiarities of Filament Visual Interaction on the Solar Disk,ity inversion lines changing their positions. The interaction between filaments depends on their internal properties, which are determined by the filament chirality, or the sign of the helicity of the filament magnetic field. In quadrupolar magnetic configurations, filaments with the same chirality

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Eruption of Prominences,ltogether. Rapidly rising prominences are called eruptive prominences. The general properties of eruptive prominences and their kinematics are considered. In most cases, there is no convincing evidence of the presence of an external source of excitation of the prominence than could lead to an erupti

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范例

Solar Jets,ons. The most numerous and ubiquitous are spicules—thin elongated structures in the solar chromosphere. Surges are larger-scale ejections than spicules, but occur much less frequently. They are usually associated with small, changing satellite sunspots. Larger-scale X-ray jets are associated with su

compose

Solar Flares,raditionally, solar flares were considered as a sudden, rapid increase in the brightness of a small area of the solar surface in white light, X-ray or EUV, lasting from a few to tens minutes. In a more general sense, solar flares are now assumed as the sudden release of magnetic energy in the solar

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Coronal Mass Ejections,a with a magnetic field within them that escape from the solar atmosphere and propagate through the heliosphere. Arriving at the Earth, the CME shakes the terrestrial magnetosphere, initiating geomagnetic storms and sometimes causing disruption to many of the achievements of the industrial and infor