Magnetic Reconnection between a Solar Jet and a Filament Channel
The solar corona is highly structured by bunches of magnetic field lines forming either loops, or twisted flux ropes representing prominences/filaments, or very dynamic structures such as jets. The aim of this paper is to understand the interaction between filament channels and jets. We use high-res...
Saved in:
| Main Authors: | , , , , , , |
|---|---|
| Format: | Article |
| Language: | English |
| Published: |
IOP Publishing
2025-01-01
|
| Series: | The Astrophysical Journal |
| Subjects: | |
| Online Access: | https://doi.org/10.3847/1538-4357/ada28e |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1832584974576910336 |
|---|---|
| author | Garima Karki Brigitte Schmieder Pooja Devi Ramesh Chandra Nicolas Labrosse Reetika Joshi Bernard Gelly |
| author_facet | Garima Karki Brigitte Schmieder Pooja Devi Ramesh Chandra Nicolas Labrosse Reetika Joshi Bernard Gelly |
| author_sort | Garima Karki |
| collection | DOAJ |
| description | The solar corona is highly structured by bunches of magnetic field lines forming either loops, or twisted flux ropes representing prominences/filaments, or very dynamic structures such as jets. The aim of this paper is to understand the interaction between filament channels and jets. We use high-resolution H α spectra obtained by the ground-based telescope Télescope Héliographique pour l'Etude du Magnétisme et des Instabilités Solaires on the Canary Islands and data from Helioseismic Magnetic Imager and Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. In this paper we present a multiwavelength study of the interaction of filaments and jets. They both consist of cool plasma embedded in magnetic structures. A jet is particularly well studied in all the AIA channels with a flow reaching 100–180 km s ^−1 . Its origin is linked to cancelling flux at the edge of the active region. Large Doppler shifts in H α are derived in a typical area for a short time (order of minute). They correspond to flows around 140 km s ^−1 . In conclusion we conjecture that these flows correspond to some interchange of magnetic field lines between the filament channel and the jets leading to cool plasmoid ejections or reconnection jets perpendicularly to the jet trajectory. |
| format | Article |
| id | doaj-art-0ae68cf3b982496ca2819281aaa8de3e |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-0ae68cf3b982496ca2819281aaa8de3e2025-01-27T06:44:07ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01979218210.3847/1538-4357/ada28eMagnetic Reconnection between a Solar Jet and a Filament ChannelGarima Karki0https://orcid.org/0009-0003-3193-7496Brigitte Schmieder1https://orcid.org/0000-0003-3364-9183Pooja Devi2https://orcid.org/0000-0003-0713-0329Ramesh Chandra3https://orcid.org/0000-0002-3518-5856Nicolas Labrosse4https://orcid.org/0000-0002-4638-157XReetika Joshi5https://orcid.org/0000-0003-0020-5754Bernard Gelly6Department of Physics, DSB Campus, Kumaun University , Nainital 263001, India ; garimakarki31@gmail.comObservatoire de Paris , LIRA, UMR8109 (CNRS), F-92195 Meudon Principal Cedex, France; Centre for mathematical Plasma Astrophysics , Department of Mathematics, KU Leuven, 3001 Leuven, Belgium; SUPA, School of Physics & Astronomy, University of Glasgow , Glasgow G12 8QQ, UKDepartment of Physics, DSB Campus, Kumaun University , Nainital 263001, India ; garimakarki31@gmail.comDepartment of Physics, DSB Campus, Kumaun University , Nainital 263001, India ; garimakarki31@gmail.comSUPA, School of Physics & Astronomy, University of Glasgow , Glasgow G12 8QQ, UKRosseland Centre for Solar Physics, University of Oslo , P.O. Box 1029 Blindern, N-0315 Oslo, Norway; Institute of Theoretical Astrophysics, University of Oslo , P.O. Box 1029 Blindern, N-0315 Oslo, NorwayTHEMIS , Tenerife, SpainThe solar corona is highly structured by bunches of magnetic field lines forming either loops, or twisted flux ropes representing prominences/filaments, or very dynamic structures such as jets. The aim of this paper is to understand the interaction between filament channels and jets. We use high-resolution H α spectra obtained by the ground-based telescope Télescope Héliographique pour l'Etude du Magnétisme et des Instabilités Solaires on the Canary Islands and data from Helioseismic Magnetic Imager and Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory. In this paper we present a multiwavelength study of the interaction of filaments and jets. They both consist of cool plasma embedded in magnetic structures. A jet is particularly well studied in all the AIA channels with a flow reaching 100–180 km s ^−1 . Its origin is linked to cancelling flux at the edge of the active region. Large Doppler shifts in H α are derived in a typical area for a short time (order of minute). They correspond to flows around 140 km s ^−1 . In conclusion we conjecture that these flows correspond to some interchange of magnetic field lines between the filament channel and the jets leading to cool plasmoid ejections or reconnection jets perpendicularly to the jet trajectory.https://doi.org/10.3847/1538-4357/ada28eSolar active regions |
| spellingShingle | Garima Karki Brigitte Schmieder Pooja Devi Ramesh Chandra Nicolas Labrosse Reetika Joshi Bernard Gelly Magnetic Reconnection between a Solar Jet and a Filament Channel The Astrophysical Journal Solar active regions |
| title | Magnetic Reconnection between a Solar Jet and a Filament Channel |
| title_full | Magnetic Reconnection between a Solar Jet and a Filament Channel |
| title_fullStr | Magnetic Reconnection between a Solar Jet and a Filament Channel |
| title_full_unstemmed | Magnetic Reconnection between a Solar Jet and a Filament Channel |
| title_short | Magnetic Reconnection between a Solar Jet and a Filament Channel |
| title_sort | magnetic reconnection between a solar jet and a filament channel |
| topic | Solar active regions |
| url | https://doi.org/10.3847/1538-4357/ada28e |
| work_keys_str_mv | AT garimakarki magneticreconnectionbetweenasolarjetandafilamentchannel AT brigitteschmieder magneticreconnectionbetweenasolarjetandafilamentchannel AT poojadevi magneticreconnectionbetweenasolarjetandafilamentchannel AT rameshchandra magneticreconnectionbetweenasolarjetandafilamentchannel AT nicolaslabrosse magneticreconnectionbetweenasolarjetandafilamentchannel AT reetikajoshi magneticreconnectionbetweenasolarjetandafilamentchannel AT bernardgelly magneticreconnectionbetweenasolarjetandafilamentchannel |