Initiation of CMEs associated with filament eruption, and the nature of CME related shocks

Файнштейн, В. Г.; Egorov, Ya. I.

doi:10.1016/j.asr.2014.05.019

Cited by 18 publications

(13 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The main stages of the CME at 09.03.2012 formation are shown in Figure 1: stage I -filament eruption (Figure 1a), stage II -formation of loop-like structures of various scales (Figure 1b), stage III -formation of the FS of the mass ejection ( Figure 1c). This sequence of the observed structures is similar to those detected earlier and characteristic of generation of CMEs with various velocities [Fainshtein V.G., et al, 2015;Grechnev V.V., et al, 2016]. Shown in Figure 1d is the profile of the mapped velocity of the CME at 09.03.2012 FS based on UV observations of the Sun, in different AIA spectral channels, as well as on LASCO data.…”

Section: Resultssupporting

confidence: 82%

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Nikitenko¹,

Lebed²,

Fedorenko³

et al. 2019

View full text Add to dashboard Cite

The Catalogues of the solar proton events [Logachev, ed., 1982-2016] provide the homogeneous data series of events with maximum intensity of > 10 MeV solar protons J ≥ 1 cm-2 s-1 sr-1 beginning from 1970 up to now. The event rates behavior is rather smooth: the total number of such events, relative to accumulated sunspot number, is almost constant in the solar cycles 21-23 and even slightly growing in the solar cycle 24. Contrary, the total number of the most powerful (GLE) events per cycle was constant within statistical errors in the cycles 21-23, and it fell abruptly in cycle 24. Considering the conventional sources of GLEs we found that production of GLEs by X-class bursts was 3 times less in cycle 24 than in cycle 23, while production of GLEs by the >1000 km/s halo-type CMEs was 5 times lower.

show abstract

Section: Resultssupporting

confidence: 82%

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Nikitenko¹,

Lebed²,

Fedorenko³

et al. 2019

View full text Add to dashboard Cite

show abstract

“…There is also a point of view that impulsive CMEs may arise from imbalance in existing magnetic ropes (see, e.g., [Temmer et al, 2008;Zagainova, Fainshtein, 2015;Eselevich et al, 2016]).…”

Section: Introductionmentioning

confidence: 99%

Features of the Initial Stage of Formation of Fast Coronal Mass Ejection on February 25, 2014

Еселевич

2020

Solar-Terrestrial Physics

View full text Add to dashboard Cite

We have analyzed the fast coronal mass ejection (CME) that occurred on February 25, 2014. The analysis is based on images taken in the 131, 211, 304, and 1700 Å UV channels of the SDO/AIA instrument and from observations obtained in the Hα line (6562.8 Å) with the telescopes of the Teide and Big Bear Observatories. The February 25, 2014 CME is associated with the ejection and subsequent explosive expansion of the magnetic flux rope, which appeared near the solar surface presumably due to the tether-cutting magnetic reconnection. The impulse of full pressure (thermal plus magnetic) resulting from such an “explosion” acts on the overlying coronal arcades, causing them to merge and form an accelerated moving frontal structure of the CME. This pressure impulse also generates a blast collisional shock wave ahead of the CME, whose velocity decreases rapidly with distance. At large distances R>7R₀ (R₀ is the solar radius) from the center of the Sun in front of the CME, a shock wave of another type is formed — a “piston” collisional shock wave whose velocity varies little with distance. At R≥15R₀, there is a transition from a collisional to a collisionless shock wave.

show abstract

“…It was shown that the altitude difference between the two structures increases with time up to 1/2AU. In (Fainshtein and Egorov, 2015), using the CME Ice-cream cone model and based on CME 3D parameters calculation technique, proposed in (Xue et al, 2005), for several CMEs observed in FOV of the Large Angle and Spectrometric Coronagraph (LASCO; Brueckner et al (1995)) onboard Solar and Heliospheric Observatory (SOHO; Domingo et al (1995)), the authors compared positions and velocities of the model CME body boundary and associated shock along the direction CME moves. It is shown that CME body and shock velocity decreases with time (with distance), and this process is faster for the body of mass ejection as compared to shock waves.…”

Section: Introductionmentioning

confidence: 99%

“…The authors have found that with time, the distance between CME front and shock increases, specifically, in FOV of STEREO/COR2 coronagraphs, and velocities of both structures in COR2 FOV go down. Note that in coronagraphs' FOV, many works estimated the ∆R parameter -shock standoff distance (distance between a CME body and associated shock on a CME axis), or standoff distance ratio ∆R/R c (the standoff distance normalized by the radius of curvature of a CME (Rc)) (for instance, see Maloney and Gallagher (2011); Gopalswamy and Yashiro (2011); Savani et al (2012); Fainshtein and Egorov (2015); Volpes and Bothmer (2016) and references therein). In (Gopalswamy and Yashiro, 2011), this parameter was derived from measurements in the FOV of LASCO coronagraphs for limb CMEs, and in (Savani et al, 2012) -from 2.5D calculations of model CME movement in the form of flux rope and associated shock.…”

Section: Introductionmentioning

confidence: 99%

Kinematics of CMEs and associated shock waves as deduced from LASCO data: comparative analysis

Fainshtein,

Egorov,

Zagainova

2017

Preprint

View full text Add to dashboard Cite

From data by LASCO C2 and C3 coronagraphs, depending on time (distance), we have determined positions and velocities of the front for fast limb CMEs' body with their sources near the limb, and for the body of halotype CME with the sources near the solar disk center. These characteristics of CME body are compared to similar kinematic characteristics obtained for CME body-associated shock waves (shocks). For the body of halo-type CME with the sources near the solar disk center and associated shocks, we determined and compared their kinematic characteristics in 3D space. It has been shown that for all the considered CME groups, the shock velocity is higher than the CME body velocity, both velocities decrease as the mass ejection moves. As this takes place, the distance between CME body and shock grows. On average, distance from CME body to shock, and velocity difference of these structures is greater for a halo CME, and even greater for a model CME in 3D.

show abstract

Initiation of CMEs associated with filament eruption, and the nature of CME related shocks

Cited by 18 publications

References 32 publications

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Book of Proceedings Tenth Workshop Primorsko, Bulgaria 2019

Features of the Initial Stage of Formation of Fast Coronal Mass Ejection on February 25, 2014

Kinematics of CMEs and associated shock waves as deduced from LASCO data: comparative analysis

Contact Info

Product

Resources

About