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

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 longitud...

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Published inAstrophysical 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
LanguageEnglish
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
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Abstract 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.
AbstractList 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 [> or =, slanted]60[degrees] 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.
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 approx. 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 greater than or equal to 60deg 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.
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.
Audience PUBLIC
Author Gopalswamy, N.
Akiyama, S.
Michalek, G.
Mäkelä, P.
Xie, H.
Yashiro, S.
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10.1029/2003JA010226
10.1002/2014GL059858
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10.1007/BF00150306
10.1029/2006JA012149
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Yashiro S. (16) 2008; 673
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Snippet 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...
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...
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SubjectTerms Abundance
Coronal mass ejection
Ejection
Flares
Halos
Heliosphere
Longitude
Soft x-rays
Solar Physics
Sun: activity
Sun: coronal mass ejections (CMEs)
Sun: flares
sunspots
Title THE PECULIAR BEHAVIOR OF HALO CORONAL MASS EJECTIONS IN SOLAR CYCLE 24
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