Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona

Coronal transients are known as sources of coronal upflows. With the commissioning of Solar Orbiter, it became apparent that coronal small-scale features are even more frequent than previously estimated. It was found that even small coronal features seen by Solar Orbiter can produce visible upflows....

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Autores: Schwanitz, Conrad, Harra, Louise, Barczynski, Krzysztof, Mandrini, Cristina H., Orozco Suárez, David, Moreno Vacas, Alejandro, Raouafi, Nour E.
Tipo de recurso: artículo
Estado:Versión publicada
Fecha de publicación:2023
País:España
Institución:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/356567
Acceso en línea:http://hdl.handle.net/10261/356567
Access Level:acceso abierto
Palabra clave:Corona
Coronal holes
Extreme-ultraviolet
Quiet
Solar wind
Spectrum
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dc.title.none.fl_str_mv Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona
title Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona
spellingShingle Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona
Schwanitz, Conrad
Corona
Coronal holes
Extreme-ultraviolet
Quiet
Solar wind
Spectrum
title_short Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona
title_full Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona
title_fullStr Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona
title_full_unstemmed Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona
title_sort Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the Corona
dc.creator.none.fl_str_mv Schwanitz, Conrad
Harra, Louise
Barczynski, Krzysztof
Mandrini, Cristina H.
Orozco Suárez, David
Moreno Vacas, Alejandro
Raouafi, Nour E.
author Schwanitz, Conrad
author_facet Schwanitz, Conrad
Harra, Louise
Barczynski, Krzysztof
Mandrini, Cristina H.
Orozco Suárez, David
Moreno Vacas, Alejandro
Raouafi, Nour E.
author_role author
author2 Harra, Louise
Barczynski, Krzysztof
Mandrini, Cristina H.
Orozco Suárez, David
Moreno Vacas, Alejandro
Raouafi, Nour E.
author2_role author
author
author
author
author
author
dc.contributor.none.fl_str_mv Federal Institute of Technology Zurich
Consejo Nacional de Investigaciones Científicas y Técnicas (Argentina)
Ministerio de Ciencia e Innovación (España)
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Corona
Coronal holes
Extreme-ultraviolet
Quiet
Solar wind
Spectrum
topic Corona
Coronal holes
Extreme-ultraviolet
Quiet
Solar wind
Spectrum
description Coronal transients are known as sources of coronal upflows. With the commissioning of Solar Orbiter, it became apparent that coronal small-scale features are even more frequent than previously estimated. It was found that even small coronal features seen by Solar Orbiter can produce visible upflows. Therefore, it is important to study the plasma flows on small scales better and understand their atmospheric driving mechanisms. In this article, we present the results from a two-week coordinated multi-spacecraft observation campaign with Hinode, IRIS, and the GREGOR telescope. We identify a small region of coronal upflows with Doppler velocities of up to 16.5 km s. The upflows are located north of a coronal bright point in a coronal hole. We study the corona, the transition region, the chromosphere and the photospheric magnetic field to find evidence of underlying mechanisms for the coronal upflow. We find a complex photospheric magnetic field with several small mixed polarities that are the footpoints of different loops. Flux emergence and cancellation are observed at the constantly changing footpoints of the coronal loops. Reconnection of loops can be identified as the driver of the coronal upflow. Furthermore, the impact of the coronal activity triggers plasma flows in the underlying layers. This work highlights that frequent small coronal features can cause considerable atmospheric response and ubiquitously produce plasma upflows that potentially feed into the solar wind. © 2023, The Author(s).
publishDate 2023
dc.date.none.fl_str_mv 2023
2024
2024
2024
dc.type.none.fl_str_mv info:eu-repo/semantics/article
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Publisher's version
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dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/356567
url http://hdl.handle.net/10261/356567
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spelling Small-Scale Upflows in a Coronal Hole – Tracked from the Photosphere to the CoronaSchwanitz, ConradHarra, LouiseBarczynski, KrzysztofMandrini, Cristina H.Orozco Suárez, DavidMoreno Vacas, AlejandroRaouafi, Nour E.CoronaCoronal holesExtreme-ultravioletQuietSolar windSpectrumCoronal transients are known as sources of coronal upflows. With the commissioning of Solar Orbiter, it became apparent that coronal small-scale features are even more frequent than previously estimated. It was found that even small coronal features seen by Solar Orbiter can produce visible upflows. Therefore, it is important to study the plasma flows on small scales better and understand their atmospheric driving mechanisms. In this article, we present the results from a two-week coordinated multi-spacecraft observation campaign with Hinode, IRIS, and the GREGOR telescope. We identify a small region of coronal upflows with Doppler velocities of up to 16.5 km s. The upflows are located north of a coronal bright point in a coronal hole. We study the corona, the transition region, the chromosphere and the photospheric magnetic field to find evidence of underlying mechanisms for the coronal upflow. We find a complex photospheric magnetic field with several small mixed polarities that are the footpoints of different loops. Flux emergence and cancellation are observed at the constantly changing footpoints of the coronal loops. Reconnection of loops can be identified as the driver of the coronal upflow. Furthermore, the impact of the coronal activity triggers plasma flows in the underlying layers. This work highlights that frequent small coronal features can cause considerable atmospheric response and ubiquitously produce plasma upflows that potentially feed into the solar wind. © 2023, The Author(s).Open access funding provided by Swiss Federal Institute of Technology Zurich. CHM acknowledges grants PICT-2020-SERIEA-03214 and PIP 11220200100985. CHM is a Senior Researcher at Consejo Nacional de Investigaciones Cientificas y Tecnicas (CONICET).DOS and AMV acknowledge funds by AEI/MCIN/10.13039/501100011033/ (RTI2018-096886-C5,PID2021-125325OB-C5, PCI2022-135009-2) and ERDF "A way of making Europe"; and "Center of Excellence Severo Ochoa" awards to IAA-CSIC (CEX2021-001131-S).r We acknowledge the use of AIA data. AIA is an instrument onboard SDO, a mission of NASA's Living With a Star program.r IRIS is a NASA small explorer mission developed and operated by LMSAL with mission operations executed at NASA Ames Research Center and major contributions to downlink communications funded by ESA and the Norwegian Space Centre.r The 1.5-meter GREGOR solar telescope was built by a German consortium under the leadership of the Leibniz-Institute for Solar Physics (KIS) in Freiburg with the Leibniz Institute for Astrophysics Potsdam, the Institute for Astrophysics Gottingen and the Max Planck Institute for Solar System Research in Gottingen as partners, and with contributions from the Instituto de Astrofisica de Canarias and the Astronomical Institute of the Academy of Sciences of the Czech Republic. The redesign of the GREGOR AO and instrument distribution optics was carried out by KIS, whose technical staff is gratefully acknowledged.Peer reviewedSpringerFederal Institute of Technology ZurichConsejo Nacional de Investigaciones Científicas y Técnicas (Argentina)Ministerio de Ciencia e Innovación (España)Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2024202420232024info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_6501Publisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/356567reponame:DIGITAL.CSIC. Repositorio Institucional del CSICinstname:Consejo Superior de Investigaciones Científicas (CSIC)Inglés#PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE##PLACEHOLDER_PARENT_METADATA_VALUE#info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/RTI2018-096886-B-C51info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PID2021-125325OB-C51info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2021-2023/PCI2022-135009-2info:eu-repo/grantAgreement/AEI/Programa Estatal para Impulsar la Investigación Científico-Técnica y su Transferencia 2021-2023/CEX2021-001131-Shttp://dx.doi.org/10.1007/s11207-023-02216-4Síinfo:eu-repo/semantics/openAccessoai:digital.csic.es:10261/3565672026-05-22T06:33:51Z
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