THE PECULIAR BEHAVIOR OF HALO CORONAL MASS EJECTIONS IN SOLAR CYCLE 24

• Published in: Astrophysical journal. Letters Vol. 804; no. 1; pp. 1 - 6
• Main Authors: Gopalswamy, N., Xie, H., Akiyama, S., Mäkelä, P., Yashiro, S., Michalek, G.
• Format: Journal Article
• Language: English
• Published: Goddard Space Flight Center The American Astronomical Society 01.05.2015; IOP Science
• Subjects: Abundance; Coronal mass ejection; Ejection; Flares; Halos; Heliosphere; Longitude; Soft x-rays; Solar Physics; Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares; sunspots; Coronal Mass Ejections; Sun
• ISSN: 2041-8205; 2041-8213; 2041-8213
• DOI: 10.1088/2041-8205/804/1/L23

ABSTRACT We report on the remarkable finding that the halo coronal mass ejections (CMEs) in cycle 24 are more abundant than in cycle 23, although the sunspot number in cycle 24 has dropped by ∼40%. We also find that the distribution of halo-CME source locations is different in cycle 24: the longitude distribution of halos is much flatter with the number of halos originating at a central meridian distance twice as large as that in cycle 23. On the other hand, the average speed and associated soft X-ray flare size are the same in both cycles, suggesting that the ambient medium into which the CMEs are ejected is significantly different. We suggest that both the higher abundance and larger central meridian longitudes of halo CMEs can be explained as a consequence of the diminished total pressure in the heliosphere in cycle 24. The reduced total pressure allows CMEs to expand more than usual making them appear as halos.