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https://olympias.lib.uoi.gr/jspui/handle/123456789/16373Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Nistico, G. | en |
| dc.contributor.author | Patsourakos, S. | en |
| dc.contributor.author | Bothmer, V. | en |
| dc.contributor.author | Zimbardo, G. | en |
| dc.date.accessioned | 2015-11-24T18:30:28Z | - |
| dc.date.available | 2015-11-24T18:30:28Z | - |
| dc.identifier.issn | 0273-1177 | - |
| dc.identifier.uri | https://olympias.lib.uoi.gr/jspui/handle/123456789/16373 | - |
| dc.rights | Default Licence | - |
| dc.subject | solar corona | en |
| dc.subject | coronal hole jets | en |
| dc.subject | euv observations | en |
| dc.subject | x-ray jets | en |
| dc.subject | earths bow shock | en |
| dc.subject | electron whistler interaction | en |
| dc.subject | background subtraction | en |
| dc.subject | solar | en |
| dc.subject | loops | en |
| dc.subject | hinode | en |
| dc.subject | secchi | en |
| dc.subject | spectrometer | en |
| dc.subject | parameters | en |
| dc.title | Determination of temperature maps of EUV coronal hole jets | en |
| heal.type | journalArticle | - |
| heal.type.en | Journal article | en |
| heal.type.el | Άρθρο Περιοδικού | el |
| heal.identifier.primary | DOI 10.1016/j.asr.2011.07.003 | - |
| heal.identifier.secondary | <Go to ISI>://000295555400004 | - |
| heal.identifier.secondary | http://ac.els-cdn.com/S0273117711005126/1-s2.0-S0273117711005126-main.pdf?_tid=196b944813708a9cc6950ac107dd9771&acdnat=1334231566_c49915de1bbac66acc5e631f58edb470 | - |
| heal.language | en | - |
| heal.access | campus | - |
| heal.recordProvider | Πανεπιστήμιο Ιωαννίνων. Σχολή Επιστημών και Τεχνολογιών. Τμήμα Βιολογικών Εφαρμογών και Τεχνολογιών | el |
| heal.publicationDate | 2011 | - |
| heal.abstract | Coronal hole jets are fast ejections of plasma occurring within coronal holes, observed at Extreme-UltraViolet (EUV) and X-ray wavelengths. Recent observations of jets by the STEREO and Hinode missions show that they are transient phenomena which occur at much higher rates than large-scale impulsive phenomena like flares and Coronal Mass Ejections (CMEs). In this paper we describe some typical characteristics of coronal jets observed by the SECCHI instruments of STEREO spacecraft. We show an example of 3D reconstruction of the helical structure for a south pole jet, and present how the angular distribution of the jet position angles changes from the Extreme-UltraViolet-Imager (EUVI) field of view to the CORonagraph1 (COR1) (height similar to 2.0 R(circle dot) heliocentric distance) field of view. Then we discuss a preliminary temperature determination for the jet plasma by using the filter ratio method at 171 and 195 angstrom and applying a technique for subtracting the EUV background radiation. The results show that jets are characterized by electron temperatures ranging between 0.8 and 1.3 MK. We present the thermal structure of the jet as temperature maps and we describe its thermal evolution. (C) 2011 COSPAR. Published by Elsevier Ltd. All rights reserved. | en |
| heal.journalName | Advances in Space Research | en |
| heal.journalType | peer reviewed | - |
| heal.fullTextAvailability | TRUE | - |
| Appears in Collections: | Άρθρα σε επιστημονικά περιοδικά ( Ανοικτά) | |
Files in This Item:
| File | Description | Size | Format | |
|---|---|---|---|---|
| Nistico-2011-Determination of tem.pdf | 2.33 MB | Adobe PDF | View/Open Request a copy |
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