Statistics of solar EUV jets

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Abstract

Collimated ejecta of matter, otherwise known as jets, are observed in large numbers in the chromosphere and lower corona of the Sun, and are of great interest in relation to their possible role for the transport of matter and energy in the solar atmosphere. These jets are subdivided into several groups characterized by different formation mechanisms and substantial variation of their characteristics. In order to distinguish separate groups of jets and identify them with respective formation mechanisms, we performed a statistical study of the full ensemble of solar extreme ultraviolet (EUV) jets using observations from the Solar Dynamics Observatory (SDO) in the 171, 193, and 304 Å channels. We identified a total of 212 such events, of which 26 % were classified as linear jets, probably generated by magnetoacoustic shocks, and 30 % as helical jets, representing small-scale filament eruptions. We found that these two groups differ significantly in their major dynamic characteristics (maximum height, initial velocity, and lifetime), as well as in their widths that are closely related to the underlying magnetic field structure, while helical jets were also shown to be much more frequently associated with the presence of hot coronal component. At the same time, we found a third class of jets with intermediate characteristics and unknown formation mechanism, requiring further study.

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About the authors

I. P. Loboda

Space Research Institute

Author for correspondence.
Email: ivan.loboda@cosmos.ru
Russian Federation, Moscow

S. A. Bogachev

Space Research Institute

Email: ivan.loboda@cosmos.ru
Russian Federation, Moscow

A. S. Kirichenko

Space Research Institute

Email: ivan.loboda@cosmos.ru
Russian Federation, Moscow

A. A. Reva

Space Research Institute

Email: ivan.loboda@cosmos.ru
Russian Federation, Moscow

A. S. Ulyanov

Space Research Institute

Email: ivan.loboda@cosmos.ru
Russian Federation, Moscow

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Supplementary files

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2. Fig. 1. Differences in the main types of solar jets by ascent height and lifetime

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3. Fig. 2. An example of observations of a jet ejection formed by a minifilament eruption in the 304 Å (a), 171 Å (b) and 193 Å (c) channels of SDO/AIA. In the 171 and 193 Å channels (b, c) the movement of cold minifilament matter is visible at the initial stage of the jet movement, while in the 193 Å channel (c) the ejection of hot coronal matter is simultaneously visible

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4. Fig. 3. Distribution of the main measured characteristics of solar jets in the VUV range. Jets registered in quiet-sun regions and coronal holes (a, b), linear and spiral jets (c–g), and jets with noticeable absorption or emission in the 171 and 193 Å channels (h–j) are shown separately

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5. Fig. 4. The strongest correlations of the measured jet characteristics. The years of observation are shown in color. The dashed lines show the linear approximations together with the corresponding values of the correlation coefficient

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6. Fig. 5. The interdependence of the lifetime and the scale expressed by the average gravitational energy for prominences and jet ejections (a), as well as for different groups of jets (b). The dashed lines show the linear approximations: red – for jet ejections, black – for prominences (a) and all types of VUV jets (b)

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