First direct observational evidence of a CME deflection by coronal hole on 15 February 2011 and a comparison with computations

Details First direct observational evidence of a CME deflection by coronal hole on 15 February 2011 and a comparison with computations First direct observational evidence of a CME deflection by coronal hole on 15 February 2011 and a comparison with computations

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh23a1950m&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SH23A-1950

Astronomy and Astrophysics

Astrophysics

[7511] Solar Physics, Astrophysics, And Astronomy / Coronal Holes, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections

Scientific paper

It has been shown that coronal holes (CHs) can deflect a coronal mass ejection (CME) away or towards the Sun-Earth line depending on their relative location (Gopalswamy et al., 2009). This effect can be described using a coronal-hole influence parameter (CHIP), which depends on the CH area, the distance between the CH and the eruption region, and the magnetic field strength within the CH at the photospheric level. We have direct observation of CME deflection during the 2011February 15 CME, which was associated with an X2.2 flare (S21W21) on 01:44 UT from STEREO/COR1 and COR2 observations. The CHIP is computed for the 2011 February 15 CME to be 0.73 G with a deflection angle of 62o. We use the 193 Å AIA image from the Solar Dynamics Observatory (SDO) for CH identification and SDO/HMI for determining the magnetic field strength inside the CH. The largest CH (centroid at S59W15)) was close to the CME eruption region (S21W21). We measured the deflection angle as 38o, using STEREO/COR2 images. This deflection angle is not too different from that obtained from the coronal hole observations.

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