J/ApJ/721/901ivo://CDS.VizieR/J/ApJ/721/901doi:10.26093/cds/vizier.17210901CDSSu Y.van Ballegooijen A.Golub L.2012-08-24T10:44:26Z2012-08-06T11:57:00ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frthe-sunx-ray-sourcesultraviolet-astronomyWe present a study of the structure and dynamics of quiescent filament channels observed by Hinode/XRT and STEREO/EUVI at the solar minimum 23/24 from 2006 November to 2008 December. For 12 channels identified on the solar disk (Group I channels), we find that the morphology of the structure on the two sides of the channel is asymmetric in both X-rays and EUV: the eastern side has curved features while the western side has straight features. We interpret the results in terms of a magnetic flux rope model. The asymmetry in the morphology is due to the variation in axial flux of the flux rope along the channel, which causes the field lines from one polarity to turn into the flux rope (curved feature), while the field lines from the other polarity are connected to very distant sources (straight). For most of the 68 channels identified by cavities at the east and west limbs (Group II channels), the asymmetry cannot be clearly identified, which is likely due to the fact that the axial flux may be relatively constant along such channels. Corresponding cavities are identified only for 5 of the 12 Group I channels, while Group II channels are identified for all of the 68 cavity pairs. The studied filament channels are often observed as dark channels in X-rays and EUV. Sheared loops within Group I channels are often seen in X-rays, but are rarely seen in Group II channels as shown in the X-ray Telescope daily synoptic observations. A survey of the dynamics of studied filament channels shows that filament eruptions occur at an average rate of 1.4 filament eruptions per channel per solar rotation.2010ApJ...721..901Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/721/901CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+AS/130/233 : WATCH Solar X-Ray Burst Catalogue (Crosby+ 1998)J/A+AS/110/99 : White-light flares models (Fang+, 1995)J/A+A/304/563 : Cool X-ray flares of Sun with GOES (Phillips+, 1995)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/721/901https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/721/901http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/721/901https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/721/901https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/721/901http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/721/901GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapX-rayUVdefaultJ/ApJ/721/901/table2Group II filament channelsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeqIndex numbermeta.id;meta.mainintDateE? Date of East limb cavity start datetime.epochnullableEXRT[1/14]? Days when East cavity is visible in XRTdtime.intervalintnullableDateW? Date of West limb cavity start datetime.epochnullableWXRT[1/18]? Days when West cavity is visible in XRTdtime.intervalintnullableDateChannel datetime.epochnullableHem/LatHemisphere and latitudepos.az.altcharS[1/4]? Channel structuresrc.class.structintnullableEruptFilament eruption date (Month(s) and day(s))time.epochcharCMECoronal mass ejection (CME) associated with Filament eruption? (Yes or No for the different eruption date(s))meta.notechar