Please use this identifier to cite or link to this item:
https://olympias.lib.uoi.gr/jspui/handle/123456789/16893Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Nindos, A. | en |
| dc.contributor.author | Andrews, M. D. | en |
| dc.date.accessioned | 2015-11-24T18:34:14Z | - |
| dc.date.available | 2015-11-24T18:34:14Z | - |
| dc.identifier.issn | 0004-637X | - |
| dc.identifier.uri | https://olympias.lib.uoi.gr/jspui/handle/123456789/16893 | - |
| dc.rights | Default Licence | - |
| dc.subject | solar-terrestrial relations | en |
| dc.subject | sun : activity | en |
| dc.subject | sun : corona | en |
| dc.subject | sun : coronal mass ejections (cmes) | en |
| dc.subject | sun : flares | en |
| dc.subject | sun : magnetic fields | en |
| dc.subject | solar active regions | en |
| dc.subject | flux ropes | en |
| dc.subject | fields | en |
| dc.subject | productivity | en |
| dc.subject | motions | en |
| dc.subject | budget | en |
| dc.subject | cmes | en |
| dc.title | The association of big flares and coronal mass ejections: What is the role of magnetic helicity? | en |
| heal.type | journalArticle | - |
| heal.type.en | Journal article | en |
| heal.type.el | Άρθρο Περιοδικού | el |
| heal.identifier.secondary | <Go to ISI>://000225418800026 | - |
| heal.identifier.secondary | http://iopscience.iop.org/1538-4357/616/2/L175/pdf/1538-4357_616_2_L175.pdf | - |
| heal.language | en | - |
| heal.access | campus | - |
| heal.recordProvider | Πανεπιστήμιο Ιωαννίνων. Σχολή Επιστημών και Τεχνολογιών. Τμήμα Βιολογικών Εφαρμογών και Τεχνολογιών | el |
| heal.publicationDate | 2004 | - |
| heal.abstract | Recently, M. D. Andrews found that approximately 40% of M-class flares between 1996 and 1999, classified according to GOES X-ray flux, are not associated with coronal mass ejections (CMEs). Using 133 events from his data set for which suitable photospheric magnetograms and coronal images were available, we studied the preflare coronal helicity of the active regions that produced big flares. The coronal magnetic field of 78 active regions was modeled under the "constant alpha" linear force-free field assumption. We find that in a statistical sense the preflare value of a and coronal helicity of the active regions producing big flares that do not have associated CMEs is smaller than the coronal helicity of those producing CME-associated big flares. A further argument supporting this conclusion is that for the active regions whose coronal magnetic field deviates from the force-free model, the change of the coronal sign of alpha within an active region is twice as likely to occur when the active region is about to produce a confined flare than a CME-associated flare. Our study indicates that the amount of the stored preflare coronal helicity may determine whether a big flare will be eruptive or confined. | en |
| heal.journalName | Astrophysical Journal | en |
| heal.journalType | peer reviewed | - |
| heal.fullTextAvailability | TRUE | - |
| Appears in Collections: | Άρθρα σε επιστημονικά περιοδικά ( Ανοικτά) | |
Files in This Item:
| File | Description | Size | Format | |
|---|---|---|---|---|
| Nindos-2004-The association of b.pdf | 269.08 kB | Adobe PDF | View/Open |
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