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https://olympias.lib.uoi.gr/jspui/handle/123456789/15845Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Dara, H. C. | en |
| dc.contributor.author | Koutchmy, S. | en |
| dc.contributor.author | Zachariadis, T. G. | en |
| dc.contributor.author | Alissandrakis, C. E. | en |
| dc.date.accessioned | 2015-11-24T17:58:39Z | - |
| dc.date.available | 2015-11-24T17:58:39Z | - |
| dc.identifier.issn | 0038-0938 | - |
| dc.identifier.uri | https://olympias.lib.uoi.gr/jspui/handle/123456789/15845 | - |
| dc.rights | Default Licence | - |
| dc.subject | high-resolution spectroscopy | en |
| dc.subject | solar atmosphere dynamics | en |
| dc.subject | small-scale topology | en |
| dc.subject | k-grains | en |
| dc.subject | 3-dimensional phenomenon | en |
| dc.subject | disk chromosphere | en |
| dc.subject | magnetic elements | en |
| dc.subject | network | en |
| dc.subject | oscillations | en |
| dc.subject | faculae | en |
| dc.title | Brightness variations of MgIb bright features | en |
| heal.type | journalArticle | - |
| heal.type.en | Journal article | en |
| heal.type.el | Άρθρο Περιοδικού | el |
| heal.identifier.secondary | <Go to ISI>://000168382700007 | - |
| heal.identifier.secondary | http://www.springerlink.com/content/j116484125788377/fulltext.pdf | - |
| heal.language | en | - |
| heal.access | campus | - |
| heal.recordProvider | Πανεπιστήμιο Ιωαννίνων. Σχολή Επιστημών και Τεχνολογιών. Τμήμα Βιολογικών Εφαρμογών και Τεχνολογιών | el |
| heal.publicationDate | 2001 | - |
| heal.abstract | We study the temporal intensity variations of MgIb bright features and investigate the corresponding Hu velocity pattern. The network bright features are well visible in the continuum, in images averaged over the duration of the observations (130 min). We detected 'flashing' bright features, which appear and disappear within two to five minutes, while the rest of the bright features undergo small variations of either their shape and/or their intensity. A power spectrum analysis reveals a 10-min oscillation fat approximately half of the stable bright features. The 5-min oscillations an detected mainly at the network boundaries, where stable bright features are located, while 3-min oscillations coincide with few bright features, but are also quite intense inside the network cells. The majority of bright features are associated with H alpha downflows. The downflow is very intense at the location of 'flashing' bright features. | 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 | |
|---|---|---|---|---|
| Dara-2001-Brightness variation.pdf | 249.02 kB | Adobe PDF | View/Open Request a copy |
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