The longitudinal inhomogeneity of the solar toroidal magnetic field generation
Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its streng...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Merzlyakov, V. L. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2015 |
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| Schlagwörter: |
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| Anmerkung: |
© Pleiades Publishing, Ltd. 2015 |
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| Übergeordnetes Werk: |
Enthalten in: Geomagnetism and aeronomy - Moscow : MAIK Nauka/Interperiodica Publ., 1996, 55(2015), 8 vom: Dez., Seite 1066-1070 |
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| Übergeordnetes Werk: |
volume:55 ; year:2015 ; number:8 ; month:12 ; pages:1066-1070 |
| Links: |
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| DOI / URN: |
10.1134/S0016793215080198 |
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| Katalog-ID: |
SPR020001436 |
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| 100 | 1 | |a Merzlyakov, V. L. |e verfasserin |4 aut | |
| 245 | 1 | 4 | |a The longitudinal inhomogeneity of the solar toroidal magnetic field generation |
| 264 | 1 | |c 2015 | |
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| 520 | |a Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. | ||
| 650 | 4 | |a Solar Activity |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Solar Cycle |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Solar Magnetic Field |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Dynamo Model |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Toroidal Field |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Starkova, L. I. |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Geomagnetism and aeronomy |d Moscow : MAIK Nauka/Interperiodica Publ., 1996 |g 55(2015), 8 vom: Dez., Seite 1066-1070 |w (DE-627)342320920 |w (DE-600)2071667-9 |x 1555-645X |7 nnns |
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| 856 | 4 | 0 | |u https://dx.doi.org/10.1134/S0016793215080198 |z lizenzpflichtig |3 Volltext |
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10.1134/S0016793215080198 doi (DE-627)SPR020001436 (SPR)S0016793215080198-e DE-627 ger DE-627 rakwb eng Merzlyakov, V. L. verfasserin aut The longitudinal inhomogeneity of the solar toroidal magnetic field generation 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. Solar Activity (dpeaa)DE-He213 Solar Cycle (dpeaa)DE-He213 Solar Magnetic Field (dpeaa)DE-He213 Dynamo Model (dpeaa)DE-He213 Toroidal Field (dpeaa)DE-He213 Starkova, L. I. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 8 vom: Dez., Seite 1066-1070 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:8 month:12 pages:1066-1070 https://dx.doi.org/10.1134/S0016793215080198 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 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_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 55 2015 8 12 1066-1070 |
| spelling |
10.1134/S0016793215080198 doi (DE-627)SPR020001436 (SPR)S0016793215080198-e DE-627 ger DE-627 rakwb eng Merzlyakov, V. L. verfasserin aut The longitudinal inhomogeneity of the solar toroidal magnetic field generation 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. Solar Activity (dpeaa)DE-He213 Solar Cycle (dpeaa)DE-He213 Solar Magnetic Field (dpeaa)DE-He213 Dynamo Model (dpeaa)DE-He213 Toroidal Field (dpeaa)DE-He213 Starkova, L. I. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 8 vom: Dez., Seite 1066-1070 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:8 month:12 pages:1066-1070 https://dx.doi.org/10.1134/S0016793215080198 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 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_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 55 2015 8 12 1066-1070 |
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10.1134/S0016793215080198 doi (DE-627)SPR020001436 (SPR)S0016793215080198-e DE-627 ger DE-627 rakwb eng Merzlyakov, V. L. verfasserin aut The longitudinal inhomogeneity of the solar toroidal magnetic field generation 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. Solar Activity (dpeaa)DE-He213 Solar Cycle (dpeaa)DE-He213 Solar Magnetic Field (dpeaa)DE-He213 Dynamo Model (dpeaa)DE-He213 Toroidal Field (dpeaa)DE-He213 Starkova, L. I. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 8 vom: Dez., Seite 1066-1070 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:8 month:12 pages:1066-1070 https://dx.doi.org/10.1134/S0016793215080198 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 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_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 55 2015 8 12 1066-1070 |
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10.1134/S0016793215080198 doi (DE-627)SPR020001436 (SPR)S0016793215080198-e DE-627 ger DE-627 rakwb eng Merzlyakov, V. L. verfasserin aut The longitudinal inhomogeneity of the solar toroidal magnetic field generation 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. Solar Activity (dpeaa)DE-He213 Solar Cycle (dpeaa)DE-He213 Solar Magnetic Field (dpeaa)DE-He213 Dynamo Model (dpeaa)DE-He213 Toroidal Field (dpeaa)DE-He213 Starkova, L. I. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 8 vom: Dez., Seite 1066-1070 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:8 month:12 pages:1066-1070 https://dx.doi.org/10.1134/S0016793215080198 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 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_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 55 2015 8 12 1066-1070 |
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10.1134/S0016793215080198 doi (DE-627)SPR020001436 (SPR)S0016793215080198-e DE-627 ger DE-627 rakwb eng Merzlyakov, V. L. verfasserin aut The longitudinal inhomogeneity of the solar toroidal magnetic field generation 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. Solar Activity (dpeaa)DE-He213 Solar Cycle (dpeaa)DE-He213 Solar Magnetic Field (dpeaa)DE-He213 Dynamo Model (dpeaa)DE-He213 Toroidal Field (dpeaa)DE-He213 Starkova, L. I. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 8 vom: Dez., Seite 1066-1070 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:8 month:12 pages:1066-1070 https://dx.doi.org/10.1134/S0016793215080198 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 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_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2070 GBV_ILN_2086 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 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_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 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_4326 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 AR 55 2015 8 12 1066-1070 |
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Merzlyakov, V. L. |
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Merzlyakov, V. L. misc Solar Activity misc Solar Cycle misc Solar Magnetic Field misc Dynamo Model misc Toroidal Field The longitudinal inhomogeneity of the solar toroidal magnetic field generation |
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The longitudinal inhomogeneity of the solar toroidal magnetic field generation Solar Activity (dpeaa)DE-He213 Solar Cycle (dpeaa)DE-He213 Solar Magnetic Field (dpeaa)DE-He213 Dynamo Model (dpeaa)DE-He213 Toroidal Field (dpeaa)DE-He213 |
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The longitudinal inhomogeneity of the solar toroidal magnetic field generation |
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The longitudinal inhomogeneity of the solar toroidal magnetic field generation |
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longitudinal inhomogeneity of the solar toroidal magnetic field generation |
| title_auth |
The longitudinal inhomogeneity of the solar toroidal magnetic field generation |
| abstract |
Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. © Pleiades Publishing, Ltd. 2015 |
| abstractGer |
Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. © Pleiades Publishing, Ltd. 2015 |
| abstract_unstemmed |
Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. The difference between the maximum and minimum can range from 4 to 10 in terms of the values of the magnetic moments of local sources of the large-scale solar magnetic field. © Pleiades Publishing, Ltd. 2015 |
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The longitudinal inhomogeneity of the solar toroidal magnetic field generation |
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https://dx.doi.org/10.1134/S0016793215080198 |
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Starkova, L. I. |
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Starkova, L. I. |
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| doi_str |
10.1134/S0016793215080198 |
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2024-07-04T03:36:48.709Z |
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L.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="4"><subfield code="a">The longitudinal inhomogeneity of the solar toroidal magnetic field generation</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2015</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="500" ind1=" " ind2=" "><subfield code="a">© Pleiades Publishing, Ltd. 2015</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract The features of the longitudinal inhomogeneity of the solar magnetic field strength in the region of its generation at mid-latitudes are investigated. For this purpose, the configuration of the large-scale magnetic field was analyzed, which is determined to the greatest extent by its strength. Model calculations have shown that the large-scale magnetic field of the Sun is created by local sources at areas where the generated magnetic field emerges. The source parameters derived from the calculations indicate a significant longitudinal variation of the analyzed field strength. The first harmonic, with one maximum and antipodal minimum, appeared to be the determining one in such a variation. The longitudinal positions of maxima and minima in the northern and southern hemispheres are the same, which indicates the simultaneousness of the generation of the solar toroidal field. 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