Magneto-isolated complexes at two levels of the solar atmosphere

Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the fo...
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Gespeichert in:

Autor*in:	Malashchuk, V. M. [verfasserIn] Stepanian, N. N. [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2013

Schlagwörter:	Sun magnetic fields chromosphere corona

Übergeordnetes Werk:	Enthalten in: Bulletin of the Crimean Astrophysical Observatory - New York, NY : Allerton Press, 2007, 109(2013), 1 vom: Juni, Seite 98-103
Übergeordnetes Werk:	volume:109 ; year:2013 ; number:1 ; month:06 ; pages:98-103

Links:	Volltext

DOI / URN:	10.3103/S0190271713010142

Katalog-ID:	SPR023524162

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allfields	10.3103/S0190271713010142 doi (DE-627)SPR023524162 (SPR)S0190271713010142-e DE-627 ger DE-627 rakwb eng 520 ASE Malashchuk, V. M. verfasserin aut Magneto-isolated complexes at two levels of the solar atmosphere 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the form of channels. Their width depends on the structures that are located close to the borders inside and outside the complex. Most arch structures with one end that is located inside the complex do not cross the boundaries of the complexes (70% at the upper chromosphere and 80% of events at the corona). A total of 80% of the coronal holes that appeared in the complexes had an open structure of the magnetic field. All these facts confirm the existence of the observed magneto-isolated complexes. It is of importance that this conclusion is derived not from the calculation of the magnetic field at different heights but from observations of structures that trace the magnetic-field lines. Sun (dpeaa)DE-He213 magnetic fields (dpeaa)DE-He213 chromosphere (dpeaa)DE-He213 corona (dpeaa)DE-He213 Stepanian, N. N. verfasserin aut Enthalten in Bulletin of the Crimean Astrophysical Observatory New York, NY : Allerton Press, 2007 109(2013), 1 vom: Juni, Seite 98-103 (DE-627)538998806 (DE-600)2380998-X 1934-7863 nnns volume:109 year:2013 number:1 month:06 pages:98-103 https://dx.doi.org/10.3103/S0190271713010142 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_63 GBV_ILN_65 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 AR 109 2013 1 06 98-103
spelling	10.3103/S0190271713010142 doi (DE-627)SPR023524162 (SPR)S0190271713010142-e DE-627 ger DE-627 rakwb eng 520 ASE Malashchuk, V. M. verfasserin aut Magneto-isolated complexes at two levels of the solar atmosphere 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the form of channels. Their width depends on the structures that are located close to the borders inside and outside the complex. Most arch structures with one end that is located inside the complex do not cross the boundaries of the complexes (70% at the upper chromosphere and 80% of events at the corona). A total of 80% of the coronal holes that appeared in the complexes had an open structure of the magnetic field. All these facts confirm the existence of the observed magneto-isolated complexes. It is of importance that this conclusion is derived not from the calculation of the magnetic field at different heights but from observations of structures that trace the magnetic-field lines. Sun (dpeaa)DE-He213 magnetic fields (dpeaa)DE-He213 chromosphere (dpeaa)DE-He213 corona (dpeaa)DE-He213 Stepanian, N. N. verfasserin aut Enthalten in Bulletin of the Crimean Astrophysical Observatory New York, NY : Allerton Press, 2007 109(2013), 1 vom: Juni, Seite 98-103 (DE-627)538998806 (DE-600)2380998-X 1934-7863 nnns volume:109 year:2013 number:1 month:06 pages:98-103 https://dx.doi.org/10.3103/S0190271713010142 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_63 GBV_ILN_65 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 AR 109 2013 1 06 98-103
allfields_unstemmed	10.3103/S0190271713010142 doi (DE-627)SPR023524162 (SPR)S0190271713010142-e DE-627 ger DE-627 rakwb eng 520 ASE Malashchuk, V. M. verfasserin aut Magneto-isolated complexes at two levels of the solar atmosphere 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the form of channels. Their width depends on the structures that are located close to the borders inside and outside the complex. Most arch structures with one end that is located inside the complex do not cross the boundaries of the complexes (70% at the upper chromosphere and 80% of events at the corona). A total of 80% of the coronal holes that appeared in the complexes had an open structure of the magnetic field. All these facts confirm the existence of the observed magneto-isolated complexes. It is of importance that this conclusion is derived not from the calculation of the magnetic field at different heights but from observations of structures that trace the magnetic-field lines. Sun (dpeaa)DE-He213 magnetic fields (dpeaa)DE-He213 chromosphere (dpeaa)DE-He213 corona (dpeaa)DE-He213 Stepanian, N. N. verfasserin aut Enthalten in Bulletin of the Crimean Astrophysical Observatory New York, NY : Allerton Press, 2007 109(2013), 1 vom: Juni, Seite 98-103 (DE-627)538998806 (DE-600)2380998-X 1934-7863 nnns volume:109 year:2013 number:1 month:06 pages:98-103 https://dx.doi.org/10.3103/S0190271713010142 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_63 GBV_ILN_65 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 AR 109 2013 1 06 98-103
allfieldsGer	10.3103/S0190271713010142 doi (DE-627)SPR023524162 (SPR)S0190271713010142-e DE-627 ger DE-627 rakwb eng 520 ASE Malashchuk, V. M. verfasserin aut Magneto-isolated complexes at two levels of the solar atmosphere 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the form of channels. Their width depends on the structures that are located close to the borders inside and outside the complex. Most arch structures with one end that is located inside the complex do not cross the boundaries of the complexes (70% at the upper chromosphere and 80% of events at the corona). A total of 80% of the coronal holes that appeared in the complexes had an open structure of the magnetic field. All these facts confirm the existence of the observed magneto-isolated complexes. It is of importance that this conclusion is derived not from the calculation of the magnetic field at different heights but from observations of structures that trace the magnetic-field lines. Sun (dpeaa)DE-He213 magnetic fields (dpeaa)DE-He213 chromosphere (dpeaa)DE-He213 corona (dpeaa)DE-He213 Stepanian, N. N. verfasserin aut Enthalten in Bulletin of the Crimean Astrophysical Observatory New York, NY : Allerton Press, 2007 109(2013), 1 vom: Juni, Seite 98-103 (DE-627)538998806 (DE-600)2380998-X 1934-7863 nnns volume:109 year:2013 number:1 month:06 pages:98-103 https://dx.doi.org/10.3103/S0190271713010142 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_63 GBV_ILN_65 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 AR 109 2013 1 06 98-103
allfieldsSound	10.3103/S0190271713010142 doi (DE-627)SPR023524162 (SPR)S0190271713010142-e DE-627 ger DE-627 rakwb eng 520 ASE Malashchuk, V. M. verfasserin aut Magneto-isolated complexes at two levels of the solar atmosphere 2013 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the form of channels. Their width depends on the structures that are located close to the borders inside and outside the complex. Most arch structures with one end that is located inside the complex do not cross the boundaries of the complexes (70% at the upper chromosphere and 80% of events at the corona). A total of 80% of the coronal holes that appeared in the complexes had an open structure of the magnetic field. All these facts confirm the existence of the observed magneto-isolated complexes. It is of importance that this conclusion is derived not from the calculation of the magnetic field at different heights but from observations of structures that trace the magnetic-field lines. Sun (dpeaa)DE-He213 magnetic fields (dpeaa)DE-He213 chromosphere (dpeaa)DE-He213 corona (dpeaa)DE-He213 Stepanian, N. N. verfasserin aut Enthalten in Bulletin of the Crimean Astrophysical Observatory New York, NY : Allerton Press, 2007 109(2013), 1 vom: Juni, Seite 98-103 (DE-627)538998806 (DE-600)2380998-X 1934-7863 nnns volume:109 year:2013 number:1 month:06 pages:98-103 https://dx.doi.org/10.3103/S0190271713010142 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_20 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_63 GBV_ILN_65 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_110 GBV_ILN_120 GBV_ILN_150 GBV_ILN_151 GBV_ILN_161 GBV_ILN_213 GBV_ILN_230 GBV_ILN_293 GBV_ILN_370 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2007 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2055 GBV_ILN_2059 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2106 GBV_ILN_2108 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2116 GBV_ILN_2118 GBV_ILN_2119 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 AR 109 2013 1 06 98-103
language	English
source	Enthalten in Bulletin of the Crimean Astrophysical Observatory 109(2013), 1 vom: Juni, Seite 98-103 volume:109 year:2013 number:1 month:06 pages:98-103
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author	Malashchuk, V. M.
spellingShingle	Malashchuk, V. M. ddc 520 misc Sun misc magnetic fields misc chromosphere misc corona Magneto-isolated complexes at two levels of the solar atmosphere
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topic_title	520 ASE Magneto-isolated complexes at two levels of the solar atmosphere Sun (dpeaa)DE-He213 magnetic fields (dpeaa)DE-He213 chromosphere (dpeaa)DE-He213 corona (dpeaa)DE-He213
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title	Magneto-isolated complexes at two levels of the solar atmosphere
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title_full	Magneto-isolated complexes at two levels of the solar atmosphere
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title_sort	magneto-isolated complexes at two levels of the solar atmosphere
title_auth	Magneto-isolated complexes at two levels of the solar atmosphere
abstract	Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the form of channels. Their width depends on the structures that are located close to the borders inside and outside the complex. Most arch structures with one end that is located inside the complex do not cross the boundaries of the complexes (70% at the upper chromosphere and 80% of events at the corona). A total of 80% of the coronal holes that appeared in the complexes had an open structure of the magnetic field. All these facts confirm the existence of the observed magneto-isolated complexes. It is of importance that this conclusion is derived not from the calculation of the magnetic field at different heights but from observations of structures that trace the magnetic-field lines.
abstractGer	Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the form of channels. Their width depends on the structures that are located close to the borders inside and outside the complex. Most arch structures with one end that is located inside the complex do not cross the boundaries of the complexes (70% at the upper chromosphere and 80% of events at the corona). A total of 80% of the coronal holes that appeared in the complexes had an open structure of the magnetic field. All these facts confirm the existence of the observed magneto-isolated complexes. It is of importance that this conclusion is derived not from the calculation of the magnetic field at different heights but from observations of structures that trace the magnetic-field lines.
abstract_unstemmed	Abstract Magneto-isolated complexes were found in the upper chromosphere from observations in the He I λ 1083 nm line. All the complexes were confidently identified in the corona from the images in the FeIX-X λ 17.1 nm line. The boundaries of the complexes at two heights are always visible in the form of channels. Their width depends on the structures that are located close to the borders inside and outside the complex. Most arch structures with one end that is located inside the complex do not cross the boundaries of the complexes (70% at the upper chromosphere and 80% of events at the corona). A total of 80% of the coronal holes that appeared in the complexes had an open structure of the magnetic field. All these facts confirm the existence of the observed magneto-isolated complexes. It is of importance that this conclusion is derived not from the calculation of the magnetic field at different heights but from observations of structures that trace the magnetic-field lines.
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title_short	Magneto-isolated complexes at two levels of the solar atmosphere
url	https://dx.doi.org/10.3103/S0190271713010142
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Magneto-isolated complexes at two levels of the solar atmosphere

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