Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE

We present imaging and spectroscopic diagnostics of a long filament during its formation with the observations from the Chinese H α Solar Explorer and Solar Dynamics Observatory. The seed filament first appeared at about 05:00 UT on 2022 September 13. Afterward, it grew gradually and connected to an...
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Autor*in:	H. T. Li [verfasserIn] X. Cheng [verfasserIn] Y. W. Ni [verfasserIn] C. Li [verfasserIn] S. H. Rao [verfasserIn] J. H. Guo [verfasserIn] M. D. Ding [verfasserIn] P. F. Chen [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Solar filaments Solar magnetic reconnection

Übergeordnetes Werk:	In: The Astrophysical Journal Letters - IOP Publishing, 2022, 958(2023), 2, p L42
Übergeordnetes Werk:	volume:958 ; year:2023 ; number:2, p L42

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/2041-8213/ad0e10

Katalog-ID:	DOAJ100142362

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520			\|a We present imaging and spectroscopic diagnostics of a long filament during its formation with the observations from the Chinese H α Solar Explorer and Solar Dynamics Observatory. The seed filament first appeared at about 05:00 UT on 2022 September 13. Afterward, it grew gradually and connected to another filament segment nearby, building up a long filament at about 20:00 UT on the same day. The CHASE H α spectra show an obvious centroid absorption with mild broadening at the main spine of the long filament, which is interpreted as evidence of filament material accumulation. More interestingly, near the footpoints of the filament, persistent redshifts have been detected in the H α spectra during the filament formation, indicating continuous drainage of filament materials. Furthermore, through inspecting the extreme-ultraviolet (EUV) images and magnetograms, it was found that EUV jets and brightenings appeared repeatedly at the junction of the two filament segments, where opposite magnetic polarities converged and canceled each other continuously. These results suggest the occurrence of intermittent magnetic reconnection that not only connects magnetic structures of the two filament segments but also supplies cold materials for the filament channel likely by the condensation of injected hot plasma, even though a part of the cold materials falls down to the filament footpoints at the same time.
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spelling	10.3847/2041-8213/ad0e10 doi (DE-627)DOAJ100142362 (DE-599)DOAJcfc06f4bed6d44f0aa640f4c69dc2d76 DE-627 ger DE-627 rakwb eng QB460-466 H. T. Li verfasserin aut Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present imaging and spectroscopic diagnostics of a long filament during its formation with the observations from the Chinese H α Solar Explorer and Solar Dynamics Observatory. The seed filament first appeared at about 05:00 UT on 2022 September 13. Afterward, it grew gradually and connected to another filament segment nearby, building up a long filament at about 20:00 UT on the same day. The CHASE H α spectra show an obvious centroid absorption with mild broadening at the main spine of the long filament, which is interpreted as evidence of filament material accumulation. More interestingly, near the footpoints of the filament, persistent redshifts have been detected in the H α spectra during the filament formation, indicating continuous drainage of filament materials. Furthermore, through inspecting the extreme-ultraviolet (EUV) images and magnetograms, it was found that EUV jets and brightenings appeared repeatedly at the junction of the two filament segments, where opposite magnetic polarities converged and canceled each other continuously. These results suggest the occurrence of intermittent magnetic reconnection that not only connects magnetic structures of the two filament segments but also supplies cold materials for the filament channel likely by the condensation of injected hot plasma, even though a part of the cold materials falls down to the filament footpoints at the same time. Solar filaments Solar magnetic reconnection Astrophysics X. Cheng verfasserin aut Y. W. Ni verfasserin aut C. Li verfasserin aut S. H. Rao verfasserin aut J. H. Guo verfasserin aut M. D. Ding verfasserin aut P. F. Chen verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 958(2023), 2, p L42 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:958 year:2023 number:2, p L42 https://doi.org/10.3847/2041-8213/ad0e10 kostenfrei https://doaj.org/article/cfc06f4bed6d44f0aa640f4c69dc2d76 kostenfrei https://doi.org/10.3847/2041-8213/ad0e10 kostenfrei https://doaj.org/toc/2041-8205 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 958 2023 2, p L42
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allfieldsSound	10.3847/2041-8213/ad0e10 doi (DE-627)DOAJ100142362 (DE-599)DOAJcfc06f4bed6d44f0aa640f4c69dc2d76 DE-627 ger DE-627 rakwb eng QB460-466 H. T. Li verfasserin aut Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present imaging and spectroscopic diagnostics of a long filament during its formation with the observations from the Chinese H α Solar Explorer and Solar Dynamics Observatory. The seed filament first appeared at about 05:00 UT on 2022 September 13. Afterward, it grew gradually and connected to another filament segment nearby, building up a long filament at about 20:00 UT on the same day. The CHASE H α spectra show an obvious centroid absorption with mild broadening at the main spine of the long filament, which is interpreted as evidence of filament material accumulation. More interestingly, near the footpoints of the filament, persistent redshifts have been detected in the H α spectra during the filament formation, indicating continuous drainage of filament materials. Furthermore, through inspecting the extreme-ultraviolet (EUV) images and magnetograms, it was found that EUV jets and brightenings appeared repeatedly at the junction of the two filament segments, where opposite magnetic polarities converged and canceled each other continuously. These results suggest the occurrence of intermittent magnetic reconnection that not only connects magnetic structures of the two filament segments but also supplies cold materials for the filament channel likely by the condensation of injected hot plasma, even though a part of the cold materials falls down to the filament footpoints at the same time. Solar filaments Solar magnetic reconnection Astrophysics X. Cheng verfasserin aut Y. W. Ni verfasserin aut C. Li verfasserin aut S. H. Rao verfasserin aut J. H. Guo verfasserin aut M. D. Ding verfasserin aut P. F. Chen verfasserin aut In The Astrophysical Journal Letters IOP Publishing, 2022 958(2023), 2, p L42 (DE-627)312189028 (DE-600)2006858-X 20418213 nnns volume:958 year:2023 number:2, p L42 https://doi.org/10.3847/2041-8213/ad0e10 kostenfrei https://doaj.org/article/cfc06f4bed6d44f0aa640f4c69dc2d76 kostenfrei https://doi.org/10.3847/2041-8213/ad0e10 kostenfrei https://doaj.org/toc/2041-8205 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 958 2023 2, p L42
language	English
source	In The Astrophysical Journal Letters 958(2023), 2, p L42 volume:958 year:2023 number:2, p L42
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topic_facet	Solar filaments Solar magnetic reconnection Astrophysics
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authorswithroles_txt_mv	H. T. Li @@aut@@ X. Cheng @@aut@@ Y. W. Ni @@aut@@ C. Li @@aut@@ S. H. Rao @@aut@@ J. H. Guo @@aut@@ M. D. Ding @@aut@@ P. F. Chen @@aut@@
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Li</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2023</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">We present imaging and spectroscopic diagnostics of a long filament during its formation with the observations from the Chinese H α Solar Explorer and Solar Dynamics Observatory. 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callnumber-first	Q - Science
author	H. T. Li
spellingShingle	H. T. Li misc QB460-466 misc Solar filaments misc Solar magnetic reconnection misc Astrophysics Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
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topic_title	QB460-466 Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE Solar filaments Solar magnetic reconnection
topic	misc QB460-466 misc Solar filaments misc Solar magnetic reconnection misc Astrophysics
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title	Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
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title_full	Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
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title_sort	formation of a long filament through the connection of two filament segments observed by chase
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title_auth	Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
abstract	We present imaging and spectroscopic diagnostics of a long filament during its formation with the observations from the Chinese H α Solar Explorer and Solar Dynamics Observatory. The seed filament first appeared at about 05:00 UT on 2022 September 13. Afterward, it grew gradually and connected to another filament segment nearby, building up a long filament at about 20:00 UT on the same day. The CHASE H α spectra show an obvious centroid absorption with mild broadening at the main spine of the long filament, which is interpreted as evidence of filament material accumulation. More interestingly, near the footpoints of the filament, persistent redshifts have been detected in the H α spectra during the filament formation, indicating continuous drainage of filament materials. Furthermore, through inspecting the extreme-ultraviolet (EUV) images and magnetograms, it was found that EUV jets and brightenings appeared repeatedly at the junction of the two filament segments, where opposite magnetic polarities converged and canceled each other continuously. These results suggest the occurrence of intermittent magnetic reconnection that not only connects magnetic structures of the two filament segments but also supplies cold materials for the filament channel likely by the condensation of injected hot plasma, even though a part of the cold materials falls down to the filament footpoints at the same time.
abstractGer	We present imaging and spectroscopic diagnostics of a long filament during its formation with the observations from the Chinese H α Solar Explorer and Solar Dynamics Observatory. The seed filament first appeared at about 05:00 UT on 2022 September 13. Afterward, it grew gradually and connected to another filament segment nearby, building up a long filament at about 20:00 UT on the same day. The CHASE H α spectra show an obvious centroid absorption with mild broadening at the main spine of the long filament, which is interpreted as evidence of filament material accumulation. More interestingly, near the footpoints of the filament, persistent redshifts have been detected in the H α spectra during the filament formation, indicating continuous drainage of filament materials. Furthermore, through inspecting the extreme-ultraviolet (EUV) images and magnetograms, it was found that EUV jets and brightenings appeared repeatedly at the junction of the two filament segments, where opposite magnetic polarities converged and canceled each other continuously. These results suggest the occurrence of intermittent magnetic reconnection that not only connects magnetic structures of the two filament segments but also supplies cold materials for the filament channel likely by the condensation of injected hot plasma, even though a part of the cold materials falls down to the filament footpoints at the same time.
abstract_unstemmed	We present imaging and spectroscopic diagnostics of a long filament during its formation with the observations from the Chinese H α Solar Explorer and Solar Dynamics Observatory. The seed filament first appeared at about 05:00 UT on 2022 September 13. Afterward, it grew gradually and connected to another filament segment nearby, building up a long filament at about 20:00 UT on the same day. The CHASE H α spectra show an obvious centroid absorption with mild broadening at the main spine of the long filament, which is interpreted as evidence of filament material accumulation. More interestingly, near the footpoints of the filament, persistent redshifts have been detected in the H α spectra during the filament formation, indicating continuous drainage of filament materials. Furthermore, through inspecting the extreme-ultraviolet (EUV) images and magnetograms, it was found that EUV jets and brightenings appeared repeatedly at the junction of the two filament segments, where opposite magnetic polarities converged and canceled each other continuously. These results suggest the occurrence of intermittent magnetic reconnection that not only connects magnetic structures of the two filament segments but also supplies cold materials for the filament channel likely by the condensation of injected hot plasma, even though a part of the cold materials falls down to the filament footpoints at the same time.
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container_issue	2, p L42
title_short	Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE
url	https://doi.org/10.3847/2041-8213/ad0e10 https://doaj.org/article/cfc06f4bed6d44f0aa640f4c69dc2d76 https://doaj.org/toc/2041-8205
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Formation of a Long Filament Through the Connection of Two Filament Segments Observed by CHASE

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