Please use this identifier to cite or link to this item:
https://olympias.lib.uoi.gr/jspui/handle/123456789/16760Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Tzatzakis, V. | en |
| dc.contributor.author | Nindos, A. | en |
| dc.contributor.author | Alissandrakis, C. E. | en |
| dc.date.accessioned | 2015-11-24T18:33:36Z | - |
| dc.date.available | 2015-11-24T18:33:36Z | - |
| dc.identifier.issn | 0038-0938 | - |
| dc.identifier.uri | https://olympias.lib.uoi.gr/jspui/handle/123456789/16760 | - |
| dc.rights | Default Licence | - |
| dc.subject | sun: corona | en |
| dc.subject | flares | en |
| dc.subject | radio radiation | en |
| dc.subject | x-rays | en |
| dc.subject | x-ray observations | en |
| dc.subject | solar-flares | en |
| dc.subject | loop | en |
| dc.subject | emission | en |
| dc.subject | bursts | en |
| dc.subject | configuration | en |
| dc.subject | wavelengths | en |
| dc.subject | electrons | en |
| dc.subject | plasma | en |
| dc.subject | field | en |
| dc.title | A Statistical Study of Microwave Flare Morphologies | en |
| heal.type | journalArticle | - |
| heal.type.en | Journal article | en |
| heal.type.el | Άρθρο Περιοδικού | el |
| heal.identifier.secondary | <Go to ISI>://000261576700005 | - |
| heal.identifier.secondary | http://www.springerlink.com/content/l47u0682483l3460/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 | This study has been motivated by the detection of a small number of optically thin microwave bursts with maximum emission near the loop top, which is contrary to the prediction of isotropic gyrosynchrotron models. Using Nobeyama Radioheliograph (NoRH) high-spatial-resolution images at 17 and 34 GHz, we study the morphology at the radio peak of 104 flares that occurred relatively close to the limb. Using data from the Nobeyama Polarimeter we were able to determine whether the 17- and 34-GHz emissions came from optically thin or thick sources. We identified single-loop events, taking into account supplementary information from EUV and soft X-ray (SXR) images. We found optically thin emission from the top of the loop in 36% of single-loop events. In agreement with standard models, in this sample 46% and 18% of the events showed optically thin emission from the footpoints and optically thick emission from the entire loop, respectively. The derived percentage of events with gyrosynchrotron emission from isotropic populations of energetic electrons is possibly an upper limit. This point is illustrated by the analysis of an optically thin event that shows footpoint emission during the rise phase and loop-top emission during the decay phase. A model that takes into account both anisotropies in the distribution function of nonthermal electrons and time evolution can reproduce the observed transition from footpoint to loop-top morphology, if electrons with pitch-angle anisotropy are injected near one of the footpoints. | 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 | |
|---|---|---|---|---|
| Tzatzakis-2008-A Statistical Study.pdf | 662.59 kB | Adobe PDF | View/Open Request a copy |
This item is licensed under a Creative Commons License
