Two-Step Filament Eruption During 14 – 15 March 2015
We present here an interesting two-step filament eruption during 14 – 15 March 2015. The filament was located in NOAA AR 12297 and associated with a halo Coronal Mass Ejection (CME). We use observations from the Atmospheric Imaging Assembly (AIA) and Heliospheric Magnetic Imager (HMI) instruments on...
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| Veröffentlicht in: | Solar physics 2017-06, Vol.292 (6), p.1, Article 81 |
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| creator | Chandra, R. Filippov, B. Joshi, R. Schmieder, B. |
| description | We present here an interesting two-step filament eruption during 14 – 15 March 2015. The filament was located in NOAA AR 12297 and associated with a halo Coronal Mass Ejection (CME). We use observations from the
Atmospheric Imaging Assembly
(AIA) and
Heliospheric Magnetic Imager
(HMI) instruments onboard the
Solar Dynamics Observatory
(SDO), and from the
Solar and Heliospheric Observatory
(SOHO)
Large Angle and Spectrometric Coronagraph
(LASCO). We also use
H
α
data from the
Global Oscillation Network Group
(GONG) telescope and the
Kanzelhoehe Solar Observatory
. The filament shows a first step eruption on 14 March 2015 and it stops its rise at a projected altitude
≈
125
Mm
on the solar disk. It remains at this height for
≈
12
hrs
. Finally it erupts on 15 March 2015 and produces a halo CME. We also find jet activity in the active region during both days, which could help the filament de-stabilization and eruption. The decay index is calculated to understand this two-step eruption. The eruption could be due to the presence of successive instability–stability–instability zones as the filament is rising. |
| doi_str_mv | 10.1007/s11207-017-1104-5 |
| format | Article |
| fullrecord | <record><control><sourceid>proquest_hal_p</sourceid><recordid>TN_cdi_hal_primary_oai_HAL_hal_02265745v1</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>1908697110</sourcerecordid><originalsourceid>FETCH-LOGICAL-c350t-50e29ec647619e513cdc7e49f6b7dfcab0bb8058595551288be577a1f6cefbb63</originalsourceid><addsrcrecordid>eNp1kLFOwzAQhi0EEqXwAGyRmBgMd0kuTtgqaClSEQNFYrMc16Gp2iTYCYitKzNv2CchURBiYTmfrO__dfoYO0W4QABx6RB9EBxQcEQIOe2xAZIIOCTB8z4bAARxt8eH7Mi5FUCXogG7mr-X_LE2lTfJ12pjitob26aq87LwbhqbFy8ehrvt52771U4k715ZvfR8QDpmB5laO3Py8w7Z02Q8v57y2cPt3fVoxnVAUHMC4ydGR6GIMDGEgV5oYcIki1KxyLRKIU1joJgSIkI_jlNDQijMIm2yNI2CITvve5dqLSubb5T9kKXK5XQ0k90f-H5EIqQ3bNmznq1s-doYV8tV2diiPU9iAnGUiNZOS2FPaVs6Z032W4sgOzGy1ylbnbLTKanN-H3GVZ0VY_80_xv6BqpHdkA</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype><pqid>1908697110</pqid></control><display><type>article</type><title>Two-Step Filament Eruption During 14 – 15 March 2015</title><source>SpringerLink Journals - AutoHoldings</source><creator>Chandra, R. ; Filippov, B. ; Joshi, R. ; Schmieder, B.</creator><creatorcontrib>Chandra, R. ; Filippov, B. ; Joshi, R. ; Schmieder, B.</creatorcontrib><description>We present here an interesting two-step filament eruption during 14 – 15 March 2015. The filament was located in NOAA AR 12297 and associated with a halo Coronal Mass Ejection (CME). We use observations from the
Atmospheric Imaging Assembly
(AIA) and
Heliospheric Magnetic Imager
(HMI) instruments onboard the
Solar Dynamics Observatory
(SDO), and from the
Solar and Heliospheric Observatory
(SOHO)
Large Angle and Spectrometric Coronagraph
(LASCO). We also use
H
α
data from the
Global Oscillation Network Group
(GONG) telescope and the
Kanzelhoehe Solar Observatory
. The filament shows a first step eruption on 14 March 2015 and it stops its rise at a projected altitude
≈
125
Mm
on the solar disk. It remains at this height for
≈
12
hrs
. Finally it erupts on 15 March 2015 and produces a halo CME. We also find jet activity in the active region during both days, which could help the filament de-stabilization and eruption. The decay index is calculated to understand this two-step eruption. The eruption could be due to the presence of successive instability–stability–instability zones as the filament is rising.</description><identifier>ISSN: 0038-0938</identifier><identifier>EISSN: 1573-093X</identifier><identifier>DOI: 10.1007/s11207-017-1104-5</identifier><language>eng</language><publisher>Dordrecht: Springer Netherlands</publisher><subject>Altitude ; Astronomical instruments ; Astrophysics ; Astrophysics and Astroparticles ; Atmospheric Sciences ; Corona ; Coronal mass ejection ; Digital imaging ; Instability ; Mathematical analysis ; Observatories ; Physics ; Physics and Astronomy ; SOHO Mission ; Solar activity ; Solar flares ; Solar observatories ; Solar oscillations ; Solar physics ; Space Exploration and Astronautics ; Space Sciences (including Extraterrestrial Physics ; Spectrometry ; Stability ; Stabilization ; Volcanoes</subject><ispartof>Solar physics, 2017-06, Vol.292 (6), p.1, Article 81</ispartof><rights>Springer Science+Business Media Dordrecht 2017</rights><rights>Solar Physics is a copyright of Springer, 2017.</rights><rights>Distributed under a Creative Commons Attribution 4.0 International License</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c350t-50e29ec647619e513cdc7e49f6b7dfcab0bb8058595551288be577a1f6cefbb63</citedby><cites>FETCH-LOGICAL-c350t-50e29ec647619e513cdc7e49f6b7dfcab0bb8058595551288be577a1f6cefbb63</cites><orcidid>0000-0003-3364-9183</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.1007/s11207-017-1104-5$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1007/s11207-017-1104-5$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>230,314,780,784,885,27924,27925,41488,42557,51319</link.rule.ids><backlink>$$Uhttps://hal.science/hal-02265745$$DView record in HAL$$Hfree_for_read</backlink></links><search><creatorcontrib>Chandra, R.</creatorcontrib><creatorcontrib>Filippov, B.</creatorcontrib><creatorcontrib>Joshi, R.</creatorcontrib><creatorcontrib>Schmieder, B.</creatorcontrib><title>Two-Step Filament Eruption During 14 – 15 March 2015</title><title>Solar physics</title><addtitle>Sol Phys</addtitle><description>We present here an interesting two-step filament eruption during 14 – 15 March 2015. The filament was located in NOAA AR 12297 and associated with a halo Coronal Mass Ejection (CME). We use observations from the
Atmospheric Imaging Assembly
(AIA) and
Heliospheric Magnetic Imager
(HMI) instruments onboard the
Solar Dynamics Observatory
(SDO), and from the
Solar and Heliospheric Observatory
(SOHO)
Large Angle and Spectrometric Coronagraph
(LASCO). We also use
H
α
data from the
Global Oscillation Network Group
(GONG) telescope and the
Kanzelhoehe Solar Observatory
. The filament shows a first step eruption on 14 March 2015 and it stops its rise at a projected altitude
≈
125
Mm
on the solar disk. It remains at this height for
≈
12
hrs
. Finally it erupts on 15 March 2015 and produces a halo CME. We also find jet activity in the active region during both days, which could help the filament de-stabilization and eruption. The decay index is calculated to understand this two-step eruption. The eruption could be due to the presence of successive instability–stability–instability zones as the filament is rising.</description><subject>Altitude</subject><subject>Astronomical instruments</subject><subject>Astrophysics</subject><subject>Astrophysics and Astroparticles</subject><subject>Atmospheric Sciences</subject><subject>Corona</subject><subject>Coronal mass ejection</subject><subject>Digital imaging</subject><subject>Instability</subject><subject>Mathematical analysis</subject><subject>Observatories</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>SOHO Mission</subject><subject>Solar activity</subject><subject>Solar flares</subject><subject>Solar observatories</subject><subject>Solar oscillations</subject><subject>Solar physics</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Spectrometry</subject><subject>Stability</subject><subject>Stabilization</subject><subject>Volcanoes</subject><issn>0038-0938</issn><issn>1573-093X</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2017</creationdate><recordtype>article</recordtype><sourceid>ABUWG</sourceid><sourceid>AFKRA</sourceid><sourceid>AZQEC</sourceid><sourceid>BENPR</sourceid><sourceid>CCPQU</sourceid><sourceid>DWQXO</sourceid><sourceid>GNUQQ</sourceid><recordid>eNp1kLFOwzAQhi0EEqXwAGyRmBgMd0kuTtgqaClSEQNFYrMc16Gp2iTYCYitKzNv2CchURBiYTmfrO__dfoYO0W4QABx6RB9EBxQcEQIOe2xAZIIOCTB8z4bAARxt8eH7Mi5FUCXogG7mr-X_LE2lTfJ12pjitob26aq87LwbhqbFy8ehrvt52771U4k715ZvfR8QDpmB5laO3Py8w7Z02Q8v57y2cPt3fVoxnVAUHMC4ydGR6GIMDGEgV5oYcIki1KxyLRKIU1joJgSIkI_jlNDQijMIm2yNI2CITvve5dqLSubb5T9kKXK5XQ0k90f-H5EIqQ3bNmznq1s-doYV8tV2diiPU9iAnGUiNZOS2FPaVs6Z032W4sgOzGy1ylbnbLTKanN-H3GVZ0VY_80_xv6BqpHdkA</recordid><startdate>20170601</startdate><enddate>20170601</enddate><creator>Chandra, R.</creator><creator>Filippov, B.</creator><creator>Joshi, R.</creator><creator>Schmieder, B.</creator><general>Springer Netherlands</general><general>Springer Nature B.V</general><general>Springer Verlag</general><scope>AAYXX</scope><scope>CITATION</scope><scope>3V.</scope><scope>7TG</scope><scope>7XB</scope><scope>88I</scope><scope>8FD</scope><scope>8FE</scope><scope>8FG</scope><scope>8FK</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>ARAPS</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>GNUQQ</scope><scope>H8D</scope><scope>HCIFZ</scope><scope>KL.</scope><scope>L7M</scope><scope>M2P</scope><scope>P5Z</scope><scope>P62</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>Q9U</scope><scope>1XC</scope><orcidid>https://orcid.org/0000-0003-3364-9183</orcidid></search><sort><creationdate>20170601</creationdate><title>Two-Step Filament Eruption During 14 – 15 March 2015</title><author>Chandra, R. ; Filippov, B. ; Joshi, R. ; Schmieder, B.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c350t-50e29ec647619e513cdc7e49f6b7dfcab0bb8058595551288be577a1f6cefbb63</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2017</creationdate><topic>Altitude</topic><topic>Astronomical instruments</topic><topic>Astrophysics</topic><topic>Astrophysics and Astroparticles</topic><topic>Atmospheric Sciences</topic><topic>Corona</topic><topic>Coronal mass ejection</topic><topic>Digital imaging</topic><topic>Instability</topic><topic>Mathematical analysis</topic><topic>Observatories</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>SOHO Mission</topic><topic>Solar activity</topic><topic>Solar flares</topic><topic>Solar observatories</topic><topic>Solar oscillations</topic><topic>Solar physics</topic><topic>Space Exploration and Astronautics</topic><topic>Space Sciences (including Extraterrestrial Physics</topic><topic>Spectrometry</topic><topic>Stability</topic><topic>Stabilization</topic><topic>Volcanoes</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Chandra, R.</creatorcontrib><creatorcontrib>Filippov, B.</creatorcontrib><creatorcontrib>Joshi, R.</creatorcontrib><creatorcontrib>Schmieder, B.</creatorcontrib><collection>CrossRef</collection><collection>ProQuest Central (Corporate)</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>ProQuest Central (purchase pre-March 2016)</collection><collection>Science Database (Alumni Edition)</collection><collection>Technology Research Database</collection><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>ProQuest Central (Alumni) (purchase pre-March 2016)</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>Advanced Technologies & Aerospace Collection</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>ProQuest Central Student</collection><collection>Aerospace Database</collection><collection>SciTech Premium Collection</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><collection>Science Database</collection><collection>Advanced Technologies & Aerospace Database</collection><collection>ProQuest Advanced Technologies & Aerospace Collection</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central Basic</collection><collection>Hyper Article en Ligne (HAL)</collection><jtitle>Solar physics</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Chandra, R.</au><au>Filippov, B.</au><au>Joshi, R.</au><au>Schmieder, B.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Two-Step Filament Eruption During 14 – 15 March 2015</atitle><jtitle>Solar physics</jtitle><stitle>Sol Phys</stitle><date>2017-06-01</date><risdate>2017</risdate><volume>292</volume><issue>6</issue><spage>1</spage><pages>1-</pages><artnum>81</artnum><issn>0038-0938</issn><eissn>1573-093X</eissn><abstract>We present here an interesting two-step filament eruption during 14 – 15 March 2015. The filament was located in NOAA AR 12297 and associated with a halo Coronal Mass Ejection (CME). We use observations from the
Atmospheric Imaging Assembly
(AIA) and
Heliospheric Magnetic Imager
(HMI) instruments onboard the
Solar Dynamics Observatory
(SDO), and from the
Solar and Heliospheric Observatory
(SOHO)
Large Angle and Spectrometric Coronagraph
(LASCO). We also use
H
α
data from the
Global Oscillation Network Group
(GONG) telescope and the
Kanzelhoehe Solar Observatory
. The filament shows a first step eruption on 14 March 2015 and it stops its rise at a projected altitude
≈
125
Mm
on the solar disk. It remains at this height for
≈
12
hrs
. Finally it erupts on 15 March 2015 and produces a halo CME. We also find jet activity in the active region during both days, which could help the filament de-stabilization and eruption. The decay index is calculated to understand this two-step eruption. The eruption could be due to the presence of successive instability–stability–instability zones as the filament is rising.</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s11207-017-1104-5</doi><orcidid>https://orcid.org/0000-0003-3364-9183</orcidid></addata></record> |
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| source | SpringerLink Journals - AutoHoldings |
| subjects | Altitude Astronomical instruments Astrophysics Astrophysics and Astroparticles Atmospheric Sciences Corona Coronal mass ejection Digital imaging Instability Mathematical analysis Observatories Physics Physics and Astronomy SOHO Mission Solar activity Solar flares Solar observatories Solar oscillations Solar physics Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Spectrometry Stability Stabilization Volcanoes |
| title | Two-Step Filament Eruption During 14 – 15 March 2015 |
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