Magnetic Flux Emergence in a Coronal Hole
A joint campaign of various space-borne and ground-based observatories, comprising the Japanese Hinode mission (Hinode Observing Plan 338, 20 – 30 September 2017), the GREGOR solar telescope, and the Vacuum Tower Telescope (VTT), investigated numerous targets such as pores, sunspots, and coronal hol...
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| Veröffentlicht in: | Solar physics 2020-05, Vol.295 (5), Article 64 |
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| creator | Palacios, Judith Utz, Dominik Hofmeister, Stefan Krikova, Kilian Gömöry, Peter Kuckein, Christoph Denker, Carsten Verma, Meetu González Manrique, Sergio Javier Campos Rozo, Jose Iván Koza, Július Temmer, Manuela Veronig, Astrid Diercke, Andrea Kontogiannis, Ioannis Cid, Consuelo |
| description | A joint campaign of various space-borne and ground-based observatories, comprising the Japanese Hinode mission (Hinode Observing Plan 338, 20 – 30 September 2017), the GREGOR solar telescope, and the Vacuum Tower Telescope (VTT), investigated numerous targets such as pores, sunspots, and coronal holes. In this study, we focus on the coronal hole region target. On 24 September 2017, a very extended non-polar coronal hole developed patches of flux emergence, which contributed to the decrease of the overall area of the coronal hole. These flux emergence patches erode the coronal hole and transform the area into a more quiet-Sun-like area, whereby bipolar magnetic structures play an important role. Conversely, flux cancellation leads to the reduction of opposite-polarity magnetic fields and to an increase in the area of the coronal hole.
Other global coronal hole characteristics, including the evolution of the associated magnetic flux and the aforementioned area evolution in the EUV, are studied using data of the Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). The interplanetary medium parameters of the solar wind display values compatible with the presence of the coronal hole. Furthermore, a particular transient is found in those parameters. |
| doi_str_mv | 10.1007/s11207-020-01629-9 |
| format | Article |
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Other global coronal hole characteristics, including the evolution of the associated magnetic flux and the aforementioned area evolution in the EUV, are studied using data of the Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). The interplanetary medium parameters of the solar wind display values compatible with the presence of the coronal hole. Furthermore, a particular transient is found in those parameters.</description><identifier>ISSN: 0038-0938</identifier><identifier>EISSN: 1573-093X</identifier><identifier>DOI: 10.1007/s11207-020-01629-9</identifier><language>eng</language><publisher>Dordrecht: Springer Netherlands</publisher><subject>Astrophysics and Astroparticles ; Atmospheric Sciences ; Coronal holes ; Datasets ; Editor’s Choice ; Evolution ; Fluctuations ; Ground-based observation ; Interplanetary medium ; Magnetic fields ; Magnetic flux ; Observatories ; Parameters ; Physics ; Physics and Astronomy ; Solar activity ; Solar observatories ; Solar physics ; Solar wind ; Space Exploration and Astronautics ; Space Sciences (including Extraterrestrial Physics ; Sun ; Sunspots ; Telescopes ; Towards Future Research on Space Weather Drivers</subject><ispartof>Solar physics, 2020-05, Vol.295 (5), Article 64</ispartof><rights>Springer Nature B.V. 2020</rights><rights>Springer Nature B.V. 2020.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c319t-980360b9ce83ae743bc81f956a9d43ab6252e8fc3ce89bec2ab3eb8e71a21a523</citedby><cites>FETCH-LOGICAL-c319t-980360b9ce83ae743bc81f956a9d43ab6252e8fc3ce89bec2ab3eb8e71a21a523</cites><orcidid>0000-0002-3242-1497 ; 0000-0002-7444-7046 ; 0000-0002-2863-3745 ; 0000-0002-0061-5916 ; 0000-0002-9858-0490 ; 0000-0002-3694-4527 ; 0000-0002-0473-4103 ; 0000-0002-7729-6415 ; 0000-0002-6546-5955 ; 0000-0003-1054-766X ; 0000-0002-1518-512X ; 0000-0002-0922-7864 ; 0000-0001-8883-6790</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/s11207-020-01629-9$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.1007/s11207-020-01629-9$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,776,780,27901,27902,41464,42533,51294</link.rule.ids></links><search><creatorcontrib>Palacios, Judith</creatorcontrib><creatorcontrib>Utz, Dominik</creatorcontrib><creatorcontrib>Hofmeister, Stefan</creatorcontrib><creatorcontrib>Krikova, Kilian</creatorcontrib><creatorcontrib>Gömöry, Peter</creatorcontrib><creatorcontrib>Kuckein, Christoph</creatorcontrib><creatorcontrib>Denker, Carsten</creatorcontrib><creatorcontrib>Verma, Meetu</creatorcontrib><creatorcontrib>González Manrique, Sergio Javier</creatorcontrib><creatorcontrib>Campos Rozo, Jose Iván</creatorcontrib><creatorcontrib>Koza, Július</creatorcontrib><creatorcontrib>Temmer, Manuela</creatorcontrib><creatorcontrib>Veronig, Astrid</creatorcontrib><creatorcontrib>Diercke, Andrea</creatorcontrib><creatorcontrib>Kontogiannis, Ioannis</creatorcontrib><creatorcontrib>Cid, Consuelo</creatorcontrib><title>Magnetic Flux Emergence in a Coronal Hole</title><title>Solar physics</title><addtitle>Sol Phys</addtitle><description>A joint campaign of various space-borne and ground-based observatories, comprising the Japanese Hinode mission (Hinode Observing Plan 338, 20 – 30 September 2017), the GREGOR solar telescope, and the Vacuum Tower Telescope (VTT), investigated numerous targets such as pores, sunspots, and coronal holes. In this study, we focus on the coronal hole region target. On 24 September 2017, a very extended non-polar coronal hole developed patches of flux emergence, which contributed to the decrease of the overall area of the coronal hole. These flux emergence patches erode the coronal hole and transform the area into a more quiet-Sun-like area, whereby bipolar magnetic structures play an important role. Conversely, flux cancellation leads to the reduction of opposite-polarity magnetic fields and to an increase in the area of the coronal hole.
Other global coronal hole characteristics, including the evolution of the associated magnetic flux and the aforementioned area evolution in the EUV, are studied using data of the Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). The interplanetary medium parameters of the solar wind display values compatible with the presence of the coronal hole. Furthermore, a particular transient is found in those parameters.</description><subject>Astrophysics and Astroparticles</subject><subject>Atmospheric Sciences</subject><subject>Coronal holes</subject><subject>Datasets</subject><subject>Editor’s Choice</subject><subject>Evolution</subject><subject>Fluctuations</subject><subject>Ground-based observation</subject><subject>Interplanetary medium</subject><subject>Magnetic fields</subject><subject>Magnetic flux</subject><subject>Observatories</subject><subject>Parameters</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Solar activity</subject><subject>Solar observatories</subject><subject>Solar physics</subject><subject>Solar wind</subject><subject>Space Exploration and Astronautics</subject><subject>Space Sciences (including Extraterrestrial Physics</subject><subject>Sun</subject><subject>Sunspots</subject><subject>Telescopes</subject><subject>Towards Future Research on Space Weather 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In this study, we focus on the coronal hole region target. On 24 September 2017, a very extended non-polar coronal hole developed patches of flux emergence, which contributed to the decrease of the overall area of the coronal hole. These flux emergence patches erode the coronal hole and transform the area into a more quiet-Sun-like area, whereby bipolar magnetic structures play an important role. Conversely, flux cancellation leads to the reduction of opposite-polarity magnetic fields and to an increase in the area of the coronal hole.
Other global coronal hole characteristics, including the evolution of the associated magnetic flux and the aforementioned area evolution in the EUV, are studied using data of the Helioseismic and Magnetic Imager (HMI) and Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). The interplanetary medium parameters of the solar wind display values compatible with the presence of the coronal hole. Furthermore, a particular transient is found in those parameters.</abstract><cop>Dordrecht</cop><pub>Springer Netherlands</pub><doi>10.1007/s11207-020-01629-9</doi><orcidid>https://orcid.org/0000-0002-3242-1497</orcidid><orcidid>https://orcid.org/0000-0002-7444-7046</orcidid><orcidid>https://orcid.org/0000-0002-2863-3745</orcidid><orcidid>https://orcid.org/0000-0002-0061-5916</orcidid><orcidid>https://orcid.org/0000-0002-9858-0490</orcidid><orcidid>https://orcid.org/0000-0002-3694-4527</orcidid><orcidid>https://orcid.org/0000-0002-0473-4103</orcidid><orcidid>https://orcid.org/0000-0002-7729-6415</orcidid><orcidid>https://orcid.org/0000-0002-6546-5955</orcidid><orcidid>https://orcid.org/0000-0003-1054-766X</orcidid><orcidid>https://orcid.org/0000-0002-1518-512X</orcidid><orcidid>https://orcid.org/0000-0002-0922-7864</orcidid><orcidid>https://orcid.org/0000-0001-8883-6790</orcidid></addata></record> |
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| subjects | Astrophysics and Astroparticles Atmospheric Sciences Coronal holes Datasets Editor’s Choice Evolution Fluctuations Ground-based observation Interplanetary medium Magnetic fields Magnetic flux Observatories Parameters Physics Physics and Astronomy Solar activity Solar observatories Solar physics Solar wind Space Exploration and Astronautics Space Sciences (including Extraterrestrial Physics Sun Sunspots Telescopes Towards Future Research on Space Weather Drivers |
| title | Magnetic Flux Emergence in a Coronal Hole |
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