Spirality of Coronal Rays

Ajabshirizadeh, A.; Filippov, B. P.

doi:10.1023/b:sola.0000035068.48435.39

Cited by 3 publications

(1 citation statement)

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“…They interpreted this as an indication of the slowing down of the shock wave front as it is pushed obliquely across the radial magnetic field lines, indicated by the deflected streamers and coronal rays. On the other hand, Ajabshirizadeh and Filippov (2004) have suggested that the magnetic field of a moving CME deflects streamer plasma from its straight radial flow. In the frame of the concept that most CMEs are created by flux rope eruptions, a CME carries rather strong electric current, which is a source of additional coronal magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Deflection of Coronal Rays by Remote CMEs: Shock Wave or Magnetic Pressure?

Filippov

Srivastava

2010

Sol Phys

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We analyze five events of the interaction of coronal mass ejections (CMEs) with the remote coronal rays located up to 90°away from the CME as observed by the SOHO/LASCO C2 coronagraph. Using sequences of SOHO/LASCO C2 images, we estimate the kink propagation in the coronal rays during their interaction with the corresponding CMEs ranging from 180 to 920 km s −1 within the interval of radial distances from 3 R to 6 R . We conclude that all studied events do not correspond to the expected pattern of shock wave propagation in the corona. Coronal ray deflection can be interpreted as the influence of the magnetic field of a moving flux rope within the CME. The motion of a large-scale flux rope away from the Sun creates changes in the structure of surrounding field lines, which are similar to the kink propagation along coronal rays. The retardation of the potential should be taken into account since the flux rope moves at a high speed, comparable with the Alfvén speed.

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Section: Introductionmentioning

confidence: 99%