On the structure and evolution of a polar crown prominence/filament system

Polar crown prominences are made of chromospheric plasma partially circling the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D dynamics of a polar crown prominence using high cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304 and 171A and the Ahead space...

Ausführliche Beschreibung

Gespeichert in:
Bibliographische Detailangaben
Veröffentlicht in:arXiv.org 2014-02
Hauptverfasser: Panesar, N K, Innes, D E, Schmit, D J, Tiwari, S K
Format: Artikel
Sprache:eng
Schlagworte:
Online-Zugang:Volltext
Tags: Tag hinzufügen
Keine Tags, Fügen Sie den ersten Tag hinzu!
container_end_page
container_issue
container_start_page
container_title arXiv.org
container_volume
creator Panesar, N K
Innes, D E
Schmit, D J
Tiwari, S K
description Polar crown prominences are made of chromospheric plasma partially circling the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D dynamics of a polar crown prominence using high cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304 and 171A and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195A. Using time series across specific structures we compare flows across the disk in 195A with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns which are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171A two-color images. We also observe intermittent but repetitious flows with velocity 15 km/s in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament linkage model.
doi_str_mv 10.48550/arxiv.1402.4989
format Article
fullrecord <record><control><sourceid>proquest_arxiv</sourceid><recordid>TN_cdi_arxiv_primary_1402_4989</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2082887368</sourcerecordid><originalsourceid>FETCH-LOGICAL-a518-8d35d5eb78e3ab179449ba00c37aaa624d6a225a3d8ef611c7d770c59aafd6bc3</originalsourceid><addsrcrecordid>eNotjztrwzAYRUWh0JBm71QEne3oacljCX2kBLJkN58lmTrYUirJafPvmzSd7nK4nIPQAyWl0FKSJcSf_lhSQVgpal3foBnjnBZaMHaHFintCSGsUkxKPkMfW4_zp8Mpx8nkKToM3mJ3DMOU--Bx6DDgQxggYhPDt8eHGMbeO2_csusHGJ3POJ1SduM9uu1gSG7xv3O0e33Zrd6LzfZtvXreFCCpLrTl0krXKu04tFTVQtQtEGK4AoCKCVsBYxK41a6rKDXKKkWMrAE6W7WGz9Hj9favsznEfoR4ai69zaX3DDxdgbPq1-RSbvZhiv6s1DCimdaKV5r_Au0MWTU</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>2082887368</pqid></control><display><type>article</type><title>On the structure and evolution of a polar crown prominence/filament system</title><source>arXiv.org</source><source>Free E- Journals</source><creator>Panesar, N K ; Innes, D E ; Schmit, D J ; Tiwari, S K</creator><creatorcontrib>Panesar, N K ; Innes, D E ; Schmit, D J ; Tiwari, S K</creatorcontrib><description>Polar crown prominences are made of chromospheric plasma partially circling the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D dynamics of a polar crown prominence using high cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304 and 171A and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195A. Using time series across specific structures we compare flows across the disk in 195A with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns which are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171A two-color images. We also observe intermittent but repetitious flows with velocity 15 km/s in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament linkage model.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1402.4989</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Color imagery ; Columns (structural) ; Evolution ; Observatories ; Physics - Solar and Stellar Astrophysics ; Prominences ; Solar activity ; Solar corona ; Solar observatories ; Topology</subject><ispartof>arXiv.org, 2014-02</ispartof><rights>2014. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.48550/arXiv.1402.4989$$DView paper in arXiv$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.1007/s11207-014-0504-z$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink></links><search><creatorcontrib>Panesar, N K</creatorcontrib><creatorcontrib>Innes, D E</creatorcontrib><creatorcontrib>Schmit, D J</creatorcontrib><creatorcontrib>Tiwari, S K</creatorcontrib><title>On the structure and evolution of a polar crown prominence/filament system</title><title>arXiv.org</title><description>Polar crown prominences are made of chromospheric plasma partially circling the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D dynamics of a polar crown prominence using high cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304 and 171A and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195A. Using time series across specific structures we compare flows across the disk in 195A with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns which are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171A two-color images. We also observe intermittent but repetitious flows with velocity 15 km/s in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament linkage model.</description><subject>Color imagery</subject><subject>Columns (structural)</subject><subject>Evolution</subject><subject>Observatories</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Prominences</subject><subject>Solar activity</subject><subject>Solar corona</subject><subject>Solar observatories</subject><subject>Topology</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2014</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotjztrwzAYRUWh0JBm71QEne3oacljCX2kBLJkN58lmTrYUirJafPvmzSd7nK4nIPQAyWl0FKSJcSf_lhSQVgpal3foBnjnBZaMHaHFintCSGsUkxKPkMfW4_zp8Mpx8nkKToM3mJ3DMOU--Bx6DDgQxggYhPDt8eHGMbeO2_csusHGJ3POJ1SduM9uu1gSG7xv3O0e33Zrd6LzfZtvXreFCCpLrTl0krXKu04tFTVQtQtEGK4AoCKCVsBYxK41a6rKDXKKkWMrAE6W7WGz9Hj9favsznEfoR4ai69zaX3DDxdgbPq1-RSbvZhiv6s1DCimdaKV5r_Au0MWTU</recordid><startdate>20140220</startdate><enddate>20140220</enddate><creator>Panesar, N K</creator><creator>Innes, D E</creator><creator>Schmit, D J</creator><creator>Tiwari, S K</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PHGZM</scope><scope>PHGZT</scope><scope>PIMPY</scope><scope>PKEHL</scope><scope>PQEST</scope><scope>PQGLB</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope><scope>GOX</scope></search><sort><creationdate>20140220</creationdate><title>On the structure and evolution of a polar crown prominence/filament system</title><author>Panesar, N K ; Innes, D E ; Schmit, D J ; Tiwari, S K</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a518-8d35d5eb78e3ab179449ba00c37aaa624d6a225a3d8ef611c7d770c59aafd6bc3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2014</creationdate><topic>Color imagery</topic><topic>Columns (structural)</topic><topic>Evolution</topic><topic>Observatories</topic><topic>Physics - Solar and Stellar Astrophysics</topic><topic>Prominences</topic><topic>Solar activity</topic><topic>Solar corona</topic><topic>Solar observatories</topic><topic>Topology</topic><toplevel>online_resources</toplevel><creatorcontrib>Panesar, N K</creatorcontrib><creatorcontrib>Innes, D E</creatorcontrib><creatorcontrib>Schmit, D J</creatorcontrib><creatorcontrib>Tiwari, S K</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science &amp; Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>ProQuest Central (New)</collection><collection>ProQuest One Academic (New)</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Middle East (New)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Applied &amp; Life Sciences</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Panesar, N K</au><au>Innes, D E</au><au>Schmit, D J</au><au>Tiwari, S K</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>On the structure and evolution of a polar crown prominence/filament system</atitle><jtitle>arXiv.org</jtitle><date>2014-02-20</date><risdate>2014</risdate><eissn>2331-8422</eissn><abstract>Polar crown prominences are made of chromospheric plasma partially circling the Suns poles between 60 and 70 degree latitude. We aim to diagnose the 3D dynamics of a polar crown prominence using high cadence EUV images from the Solar Dynamics Observatory (SDO)/AIA at 304 and 171A and the Ahead spacecraft of the Solar Terrestrial Relations Observatory (STEREO-A)/EUVI at 195A. Using time series across specific structures we compare flows across the disk in 195A with the prominence dynamics seen on the limb. The densest prominence material forms vertical columns which are separated by many tens of Mm and connected by dynamic bridges of plasma that are clearly visible in 304/171A two-color images. We also observe intermittent but repetitious flows with velocity 15 km/s in the prominence that appear to be associated with EUV bright points on the solar disk. The boundary between the prominence and the overlying cavity appears as a sharp edge. We discuss the structure of the coronal cavity seen both above and around the prominence. SDO/HMI and GONG magnetograms are used to infer the underlying magnetic topology. The evolution and structure of the prominence with respect to the magnetic field seems to agree with the filament linkage model.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.1402.4989</doi><oa>free_for_read</oa></addata></record>
fulltext fulltext
identifier EISSN: 2331-8422
ispartof arXiv.org, 2014-02
issn 2331-8422
language eng
recordid cdi_arxiv_primary_1402_4989
source arXiv.org; Free E- Journals
subjects Color imagery
Columns (structural)
Evolution
Observatories
Physics - Solar and Stellar Astrophysics
Prominences
Solar activity
Solar corona
Solar observatories
Topology
title On the structure and evolution of a polar crown prominence/filament system
url https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-15T16%3A26%3A24IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_arxiv&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=On%20the%20structure%20and%20evolution%20of%20a%20polar%20crown%20prominence/filament%20system&rft.jtitle=arXiv.org&rft.au=Panesar,%20N%20K&rft.date=2014-02-20&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.1402.4989&rft_dat=%3Cproquest_arxiv%3E2082887368%3C/proquest_arxiv%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2082887368&rft_id=info:pmid/&rfr_iscdi=true