Kinematic characteristics of stealth CME in three-dimensional space-Reference-Cited by-同舟云学术

Kinematic characteristics of stealth CME in three-dimensional space

Published:2022-09-30 Issue:3 Volume:8 Page:13-21
ISSN:2500-0535
Container-title:Solar-Terrestrial Physics
language:en
Short-container-title:

Author:

Egorov Yaroslav¹,Fainshtein Victor¹

Affiliation:

1. Institute of Solar Terrestrial Physics SB RAS

Abstract

We have studied and compared kinematic characteristics of the motion of coronal mass ejections (CMEs) in three-dimensional (3D) space for three groups of CMEs for the period 2008–2014. These CME groups include: (i) stealth CMEs, (ii) CMEs that originate on the front side of the Sun (for an observer on Earth) and are associated with X-ray flares and filament eruption, (iii) all CMEs registered during the given period. Stealth CMEs are CMEs that emerge on the front side of the Sun and are unrelated to X-ray flares, as well as to filament eruption. We compare kinematic and some physical characteristics of these CMEs with those of a separate group of CMEs, classified as stealth in [D’Huys et al., 2014]. After comparing the characteristics of the three CME groups (i)–(iii), we concluded that stealth CMEs have, on average, the lowest velocity, kinetic energy, mass and angular size, central position angle, and also the angle φ between the direction of CME motion in the ecliptic plane and the Sun–Earth line and the angle λ between the direction of CME motion in 3D space and the ecliptic plane. We also discuss distributions of CMEs of different types by kinematic characteristics.

Publisher

Infra-M Academic Publishing House

Subject

Space and Planetary Science,Atmospheric Science,Geophysics

Reference16 articles.

1. Alzate N., Morgan H. Identification of low coronal sources of stealth coronal mass ejections using new image processing techniques. Astrophys. J. 2017, vol. 840, article id. 103, 14 p. DOI: 10.3847/1538-4357/aa6caa., Alzate N., Morgan H. Identification of low coronal sources of stealth coronal mass ejections using new image processing techniques. Astrophys. J. 2017, vol. 840, article id. 103, 14 p. DOI: 10.3847/1538-4357/aa6caa.

2. Brueckner G.E., Howard R.A., Koomen M.J., Korendyke C.M., Michels D.J., Moses J.D., Socker D.G., et al. The Large Angle Spectroscopic Coronagraph (LASCO). Solar Phys. 1995, vol. 162, p. 357. DOI: 10.1007/BF00733434., Brueckner G.E., Howard R.A., Koomen M.J., Korendyke C.M., Michels D.J., Moses J.D., Socker D.G., et al. The Large Angle Spectroscopic Coronagraph (LASCO). Solar Phys. 1995, vol. 162, p. 357. DOI: 10.1007/BF00733434.

3. D’Huys E., Seation D., Poedts S., Berghmans D. Visualizing fuzzy overlapping communities in networks. Astrophys. J. 2014, vol. 795, iss. 1, article id. 49, 12 p. DOI: 10.1088/0004-637X/795/1/49., D’Huys E., Seation D., Poedts S., Berghmans D. Visualizing fuzzy overlapping communities in networks. Astrophys. J. 2014, vol. 795, iss. 1, article id. 49, 12 p. DOI: 10.1088/0004-637X/795/1/49.

4. Egorov Ya.I., Fainshtein V.G. A simple technique for identifying the propagation direction of CME in a 3D space. Solar Phys. 2021, vol. 296, iss. 9, article id. 126, 14 p. DOI: 10.1007/s11207-021-01904-3., Egorov Ya.I., Fainshtein V.G. A simple technique for identifying the propagation direction of CME in a 3D space. Solar Phys. 2021, vol. 296, iss. 9, article id. 126, 14 p. DOI: 10.1007/s11207-021-01904-3.

5. Fainshtein V.G., Egorov Ya.I. Initiation of CMEs associated with filament eruption, and the nature of CME related shocks. Adv. Space Res. 2015, vol. 55, iss. 3, рр. 798–807. DOI: 10.1016/j.asr.2014.05.019., Fainshtein V.G., Egorov Ya.I. Initiation of CMEs associated with filament eruption, and the nature of CME related shocks. Adv. Space Res. 2015, vol. 55, iss. 3, rr. 798–807. DOI: 10.1016/j.asr.2014.05.019.