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https://olympias.lib.uoi.gr/jspui/handle/123456789/17285Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Nindos, A. | en |
| dc.contributor.author | Aurass, H. | en |
| dc.contributor.author | Klein, K. L. | en |
| dc.contributor.author | Trottet, G. | en |
| dc.date.accessioned | 2015-11-24T18:38:08Z | - |
| dc.date.available | 2015-11-24T18:38:08Z | - |
| dc.identifier.issn | 0038-0938 | - |
| dc.identifier.uri | https://olympias.lib.uoi.gr/jspui/handle/123456789/17285 | - |
| dc.rights | Default Licence | - |
| dc.subject | sun | en |
| dc.subject | flares | en |
| dc.subject | coronal mass ejections | en |
| dc.subject | radio radiation | en |
| dc.subject | corona | en |
| dc.subject | hard x-ray | en |
| dc.subject | solar microwave-bursts | en |
| dc.subject | anisotropic electron distributions | en |
| dc.subject | slowly drifting structures | en |
| dc.subject | energetic particle event | en |
| dc.subject | spectral fine-structures | en |
| dc.subject | narrow-band spikes | en |
| dc.subject | shock-waves | en |
| dc.subject | iii bursts | en |
| dc.subject | gyrosynchrotron emission | en |
| dc.title | Radio Emission of Flares and Coronal Mass Ejections Invited Review | en |
| heal.type | journalArticle | - |
| heal.type.en | Journal article | en |
| heal.type.el | Άρθρο Περιοδικού | el |
| heal.identifier.primary | DOI 10.1007/s11207-008-9258-9 | - |
| heal.identifier.secondary | <Go to ISI>://000261576700002 | - |
| heal.identifier.secondary | http://www.springerlink.com/content/c18m94u76q411862/fulltext.pdf | - |
| heal.language | en | - |
| heal.access | campus | - |
| heal.recordProvider | Πανεπιστήμιο Ιωαννίνων. Σχολή Επιστημών και Τεχνολογιών. Τμήμα Βιολογικών Εφαρμογών και Τεχνολογιών | el |
| heal.publicationDate | 2008 | - |
| heal.abstract | We review recent progress on our understanding of radio emission from solar flares and coronal mass ejections (CMEs) with emphasis on those aspects of the subject that help us address questions about energy release and its properties, the configuration of flare CME source regions, coronal shocks, particle acceleration and transport, and the origin of solar energetic particle (SEP) events. Radio emission from electron beams can provide information about the electron acceleration process, the location of injection of electrons in the corona, and the properties of the ambient coronal structures. Mildly relativistic electrons gyrating in the magnetic fields of flaring loops produce radio emission via the gyrosynchrotron mechanism, which provides constraints on the magnetic field and the properties of energetic electrons. CME detection at radio wavelengths tracks the eruption from its early phase and reveals the participation of a multitude of loops of widely differing scale. Both flares and CMEs can ignite shock waves and radio observations offer the most robust tool to study them. The incorporation of radio data into the study of SEP events reveals that a clear-cut distinction between flare-related and CME-related SEP events is difficult to establish. | en |
| heal.journalName | Solar Physics | 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-2008-Radio Emission of Fl.pdf | 1.29 MB | Adobe PDF | View/Open Request a copy |
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