Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere
Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain paramete...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Smolin, S. V. [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), 2 vom: März, Seite 166-173 |
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| Übergeordnetes Werk: |
volume:55 ; year:2015 ; number:2 ; month:03 ; pages:166-173 |
| Links: |
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| DOI / URN: |
10.1134/S0016793215020152 |
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| Katalog-ID: |
SPR020000227 |
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| 100 | 1 | |a Smolin, S. V. |e verfasserin |4 aut | |
| 245 | 1 | 0 | |a Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere |
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| 520 | |a Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. | ||
| 650 | 4 | |a Pitch Angle |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Magnetic Storm |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Radiation Belt |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Phase Space Density |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Pitch Angle Distribution |7 (dpeaa)DE-He213 | |
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| 856 | 4 | 0 | |u https://dx.doi.org/10.1134/S0016793215020152 |z lizenzpflichtig |3 Volltext |
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10.1134/S0016793215020152 doi (DE-627)SPR020000227 (SPR)S0016793215020152-e DE-627 ger DE-627 rakwb eng Smolin, S. V. verfasserin aut Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. Pitch Angle (dpeaa)DE-He213 Magnetic Storm (dpeaa)DE-He213 Radiation Belt (dpeaa)DE-He213 Phase Space Density (dpeaa)DE-He213 Pitch Angle Distribution (dpeaa)DE-He213 Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 166-173 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:166-173 https://dx.doi.org/10.1134/S0016793215020152 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 2 03 166-173 |
| spelling |
10.1134/S0016793215020152 doi (DE-627)SPR020000227 (SPR)S0016793215020152-e DE-627 ger DE-627 rakwb eng Smolin, S. V. verfasserin aut Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. Pitch Angle (dpeaa)DE-He213 Magnetic Storm (dpeaa)DE-He213 Radiation Belt (dpeaa)DE-He213 Phase Space Density (dpeaa)DE-He213 Pitch Angle Distribution (dpeaa)DE-He213 Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 166-173 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:166-173 https://dx.doi.org/10.1134/S0016793215020152 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 2 03 166-173 |
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10.1134/S0016793215020152 doi (DE-627)SPR020000227 (SPR)S0016793215020152-e DE-627 ger DE-627 rakwb eng Smolin, S. V. verfasserin aut Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. Pitch Angle (dpeaa)DE-He213 Magnetic Storm (dpeaa)DE-He213 Radiation Belt (dpeaa)DE-He213 Phase Space Density (dpeaa)DE-He213 Pitch Angle Distribution (dpeaa)DE-He213 Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 166-173 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:166-173 https://dx.doi.org/10.1134/S0016793215020152 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 2 03 166-173 |
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10.1134/S0016793215020152 doi (DE-627)SPR020000227 (SPR)S0016793215020152-e DE-627 ger DE-627 rakwb eng Smolin, S. V. verfasserin aut Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. Pitch Angle (dpeaa)DE-He213 Magnetic Storm (dpeaa)DE-He213 Radiation Belt (dpeaa)DE-He213 Phase Space Density (dpeaa)DE-He213 Pitch Angle Distribution (dpeaa)DE-He213 Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 166-173 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:166-173 https://dx.doi.org/10.1134/S0016793215020152 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 2 03 166-173 |
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10.1134/S0016793215020152 doi (DE-627)SPR020000227 (SPR)S0016793215020152-e DE-627 ger DE-627 rakwb eng Smolin, S. V. verfasserin aut Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. Pitch Angle (dpeaa)DE-He213 Magnetic Storm (dpeaa)DE-He213 Radiation Belt (dpeaa)DE-He213 Phase Space Density (dpeaa)DE-He213 Pitch Angle Distribution (dpeaa)DE-He213 Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 166-173 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:166-173 https://dx.doi.org/10.1134/S0016793215020152 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 2 03 166-173 |
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Enthalten in Geomagnetism and aeronomy 55(2015), 2 vom: März, Seite 166-173 volume:55 year:2015 number:2 month:03 pages:166-173 |
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| author |
Smolin, S. V. |
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Smolin, S. V. misc Pitch Angle misc Magnetic Storm misc Radiation Belt misc Phase Space Density misc Pitch Angle Distribution Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere |
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Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere Pitch Angle (dpeaa)DE-He213 Magnetic Storm (dpeaa)DE-He213 Radiation Belt (dpeaa)DE-He213 Phase Space Density (dpeaa)DE-He213 Pitch Angle Distribution (dpeaa)DE-He213 |
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Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere |
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modeling the pitch angle distribution on the nightside of the earth’s magnetosphere |
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Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere |
| abstract |
Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. © Pleiades Publishing, Ltd. 2015 |
| abstractGer |
Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. © Pleiades Publishing, Ltd. 2015 |
| abstract_unstemmed |
Abstract A mathematical model has been proposed for the diffusion pitch angle distribution in the magnetosphere. It makes it possible to calculate theoretically the phase space density (or the pitch angle distribution) of charged particles depending on the particle mass and energy, McIlwain parameter, magnetic local time, initial perpendicular value of the particle pitch angle distribution parameter ($ γ_{⊥0} $), variable parameter k characterizing the wave-particle interaction time, and magnetic activity index Kp. The model describes all four main types of pitch angle distributions, together with their variations, and simultaneously takes into account the possible physical mechanisms by which “butterfly” pitch angle distributions are formed as a wave-particle interaction, particle injection and drift, and splitting of the electric field drift shell. The potential of the proposed pitch angle diffusion model in the Earth’s magnetosphere has been demonstrated, as exemplified by the pitch angle distribution evolution over the last 68 hours of the magnetic storm that occurred on May 1–7, 1998. The model was quantitatively tested by a comparison of the calculated proton fluxes with the Polar/MICS spacecraft measurements during the magnetic storm of October 21–22, 1999. Good agreement between the calculated pitch angle distribution and the experimental data was obtained. © Pleiades Publishing, Ltd. 2015 |
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Modeling the pitch angle distribution on the nightside of the Earth’s magnetosphere |
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