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...
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| creator | Karki, Garima Schmieder, Brigitte Devi, Pooja Chandra, Ramesh Labrosse, Nicolas Joshi, Reetika Gelly, Bernard |
| 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$\alpha$ spectra obtained by the ground-based Telescope Heliographique pour
lEtude du Magnetisme et des Instabilites Solaires (THEMIS) in Canary Islands,
and data from Helioseismic Magnetic Imager (HMI) and Atmospheric Imaging
Assembly (AIA) aboard the Solar Dynamics Observatory (SDO). In this paper we
present a multi-wavelength 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 Dopplershifts in H$\alpha$ are derived in a typical area for a
short time (order of min). 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. |
| doi_str_mv | 10.48550/arxiv.2412.09206 |
| format | Article |
| fullrecord | <record><control><sourceid>arxiv_GOX</sourceid><recordid>TN_cdi_arxiv_primary_2412_09206</recordid><sourceformat>XML</sourceformat><sourcesystem>PC</sourcesystem><sourcerecordid>2412_09206</sourcerecordid><originalsourceid>FETCH-arxiv_primary_2412_092063</originalsourceid><addsrcrecordid>eNpjYJA0NNAzsTA1NdBPLKrILNMzMjE00jOwNDIw42Rw8E1Mz0styUxWCEpNzs_LS00uyczPU0hKLSlPTc1TSFQIzs9JLFLwSi1RSMxLAfLdMnMSc1PzShScMxKBynN4GFjTEnOKU3mhNDeDvJtriLOHLtiu-IKizNzEosp4kJ3xYDuNCasAAKF5Nd0</addsrcrecordid><sourcetype>Open Access Repository</sourcetype><iscdi>true</iscdi><recordtype>article</recordtype></control><display><type>article</type><title>Magnetic Reconnection between a Solar Jet and a Filament Channel</title><source>arXiv.org</source><creator>Karki, Garima ; Schmieder, Brigitte ; Devi, Pooja ; Chandra, Ramesh ; Labrosse, Nicolas ; Joshi, Reetika ; Gelly, Bernard</creator><creatorcontrib>Karki, Garima ; Schmieder, Brigitte ; Devi, Pooja ; Chandra, Ramesh ; Labrosse, Nicolas ; Joshi, Reetika ; Gelly, Bernard</creatorcontrib><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$\alpha$ spectra obtained by the ground-based Telescope Heliographique pour
lEtude du Magnetisme et des Instabilites Solaires (THEMIS) in Canary Islands,
and data from Helioseismic Magnetic Imager (HMI) and Atmospheric Imaging
Assembly (AIA) aboard the Solar Dynamics Observatory (SDO). In this paper we
present a multi-wavelength 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 Dopplershifts in H$\alpha$ are derived in a typical area for a
short time (order of min). 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.</description><identifier>DOI: 10.48550/arxiv.2412.09206</identifier><language>eng</language><subject>Physics - Solar and Stellar Astrophysics</subject><creationdate>2024-12</creationdate><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,777,882</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/2412.09206$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.2412.09206$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Karki, Garima</creatorcontrib><creatorcontrib>Schmieder, Brigitte</creatorcontrib><creatorcontrib>Devi, Pooja</creatorcontrib><creatorcontrib>Chandra, Ramesh</creatorcontrib><creatorcontrib>Labrosse, Nicolas</creatorcontrib><creatorcontrib>Joshi, Reetika</creatorcontrib><creatorcontrib>Gelly, Bernard</creatorcontrib><title>Magnetic Reconnection between a Solar Jet and a Filament Channel</title><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$\alpha$ spectra obtained by the ground-based Telescope Heliographique pour
lEtude du Magnetisme et des Instabilites Solaires (THEMIS) in Canary Islands,
and data from Helioseismic Magnetic Imager (HMI) and Atmospheric Imaging
Assembly (AIA) aboard the Solar Dynamics Observatory (SDO). In this paper we
present a multi-wavelength 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 Dopplershifts in H$\alpha$ are derived in a typical area for a
short time (order of min). 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.</description><subject>Physics - Solar and Stellar Astrophysics</subject><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2024</creationdate><recordtype>article</recordtype><sourceid>GOX</sourceid><recordid>eNpjYJA0NNAzsTA1NdBPLKrILNMzMjE00jOwNDIw42Rw8E1Mz0styUxWCEpNzs_LS00uyczPU0hKLSlPTc1TSFQIzs9JLFLwSi1RSMxLAfLdMnMSc1PzShScMxKBynN4GFjTEnOKU3mhNDeDvJtriLOHLtiu-IKizNzEosp4kJ3xYDuNCasAAKF5Nd0</recordid><startdate>20241212</startdate><enddate>20241212</enddate><creator>Karki, Garima</creator><creator>Schmieder, Brigitte</creator><creator>Devi, Pooja</creator><creator>Chandra, Ramesh</creator><creator>Labrosse, Nicolas</creator><creator>Joshi, Reetika</creator><creator>Gelly, Bernard</creator><scope>GOX</scope></search><sort><creationdate>20241212</creationdate><title>Magnetic Reconnection between a Solar Jet and a Filament Channel</title><author>Karki, Garima ; Schmieder, Brigitte ; Devi, Pooja ; Chandra, Ramesh ; Labrosse, Nicolas ; Joshi, Reetika ; Gelly, Bernard</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-arxiv_primary_2412_092063</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2024</creationdate><topic>Physics - Solar and Stellar Astrophysics</topic><toplevel>online_resources</toplevel><creatorcontrib>Karki, Garima</creatorcontrib><creatorcontrib>Schmieder, Brigitte</creatorcontrib><creatorcontrib>Devi, Pooja</creatorcontrib><creatorcontrib>Chandra, Ramesh</creatorcontrib><creatorcontrib>Labrosse, Nicolas</creatorcontrib><creatorcontrib>Joshi, Reetika</creatorcontrib><creatorcontrib>Gelly, Bernard</creatorcontrib><collection>arXiv.org</collection></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Karki, Garima</au><au>Schmieder, Brigitte</au><au>Devi, Pooja</au><au>Chandra, Ramesh</au><au>Labrosse, Nicolas</au><au>Joshi, Reetika</au><au>Gelly, Bernard</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Magnetic Reconnection between a Solar Jet and a Filament Channel</atitle><date>2024-12-12</date><risdate>2024</risdate><abstract>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$\alpha$ spectra obtained by the ground-based Telescope Heliographique pour
lEtude du Magnetisme et des Instabilites Solaires (THEMIS) in Canary Islands,
and data from Helioseismic Magnetic Imager (HMI) and Atmospheric Imaging
Assembly (AIA) aboard the Solar Dynamics Observatory (SDO). In this paper we
present a multi-wavelength 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 Dopplershifts in H$\alpha$ are derived in a typical area for a
short time (order of min). 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.</abstract><doi>10.48550/arxiv.2412.09206</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Physics - Solar and Stellar Astrophysics |
| title | Magnetic Reconnection between a Solar Jet and a Filament Channel |
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