The relation between coronal holes and coronal mass ejections during the rise, maximum, and declining phases of Solar Cycle 23

Details The relation between coronal holes and coronal mass ejections during the rise, maximum, and declining phases of Solar Cycle 23 The relation between coronal holes and coronal mass ejections during the rise, maximum, and declining phases of Solar Cycle 23

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012jgra..11701103m&link_type=abstract

Journal of Geophysical Research, Volume 117, Issue A1, CiteID A01103

Physics

Natural Hazards: Space Weather (2101, 2788, 7900), Radio Science: Magnetospheric Physics (2700)

Scientific paper

We study the interaction between coronal holes (CHs) and coronal mass ejections (CMEs) using a resultant force exerted by all the coronal holes present on the disk and is defined as the coronal hole influence parameter (CHIP). The CHIP magnitude for each CH depends on the CH area, the distance between the CH centroid and the eruption region, and the average magnetic field within the CH at the photospheric level. The CHIP direction for each CH points from the CH centroid to the eruption region. We focus on Solar Cycle 23 CMEs originating from the disk center of the Sun (central meridian distance ≤15°) and resulting in magnetic clouds (MCs) and non-MCs in the solar wind. The CHIP is found to be the smallest during the rise phase for MCs and non-MCs. The maximum phase has the largest CHIP value (2.9 G) for non-MCs. The CHIP is the largest (5.8 G) for driverless (DL) shocks, which are shocks at 1 AU with no discernible MC or non-MC. These results suggest that the behavior of non-MCs is similar to that of the DL shocks and different from that of MCs. In other words, the CHs may deflect the CMEs away from the Sun-Earth line and force them to behave like limb CMEs with DL shocks. This finding supports the idea that all CMEs may be flux ropes if viewed from an appropriate vantage point.

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