The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions

Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetosp...
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Autor*in:	Feygin, F. Z. [verfasserIn] Khabazin, Yu. G. Kleimenova, N. G. Malysheva, L. M. Raita, T.

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2015

Schlagwörter:	Wave Packet EMIC Wave Energetic Proton Narrow Frequency Band Outer Radiation Belt

Anmerkung:	© Pleiades Publishing, Ltd. 2015

Übergeordnetes Werk:	Enthalten in: Geomagnetism and aeronomy - Moscow : MAIK Nauka/Interperiodica Publ., 1996, 55(2015), 2 vom: März, Seite 185-191
Übergeordnetes Werk:	volume:55 ; year:2015 ; number:2 ; month:03 ; pages:185-191

Links:	Volltext

DOI / URN:	10.1134/S0016793215020048

Katalog-ID:	SPR020000251

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100	1		\|a Feygin, F. Z. \|e verfasserin \|4 aut
245	1	4	\|a The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions
264		1	\|c 2015
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520			\|a Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere.
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650		4	\|a EMIC Wave \|7 (dpeaa)DE-He213
650		4	\|a Energetic Proton \|7 (dpeaa)DE-He213
650		4	\|a Narrow Frequency Band \|7 (dpeaa)DE-He213
650		4	\|a Outer Radiation Belt \|7 (dpeaa)DE-He213
700	1		\|a Khabazin, Yu. G. \|4 aut
700	1		\|a Kleimenova, N. G. \|4 aut
700	1		\|a Malysheva, L. M. \|4 aut
700	1		\|a Raita, T. \|4 aut
773	0	8	\|i Enthalten in \|t Geomagnetism and aeronomy \|d Moscow : MAIK Nauka/Interperiodica Publ., 1996 \|g 55(2015), 2 vom: März, Seite 185-191 \|w (DE-627)342320920 \|w (DE-600)2071667-9 \|x 1555-645X \|7 nnns
773	1	8	\|g volume:55 \|g year:2015 \|g number:2 \|g month:03 \|g pages:185-191
856	4	0	\|u https://dx.doi.org/10.1134/S0016793215020048 \|z lizenzpflichtig \|3 Volltext
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912			\|a GBV_ILN_22
912			\|a GBV_ILN_23
912			\|a GBV_ILN_24
912			\|a GBV_ILN_31
912			\|a GBV_ILN_32
912			\|a GBV_ILN_39
912			\|a GBV_ILN_40
912			\|a GBV_ILN_60
912			\|a GBV_ILN_62
912			\|a GBV_ILN_63
912			\|a GBV_ILN_65
912			\|a GBV_ILN_69
912			\|a GBV_ILN_70
912			\|a GBV_ILN_73
912			\|a GBV_ILN_74
912			\|a GBV_ILN_90
912			\|a GBV_ILN_95
912			\|a GBV_ILN_100
912			\|a GBV_ILN_105
912			\|a GBV_ILN_110
912			\|a GBV_ILN_120
912			\|a GBV_ILN_138
912			\|a GBV_ILN_150
912			\|a GBV_ILN_151
912			\|a GBV_ILN_152
912			\|a GBV_ILN_161
912			\|a GBV_ILN_170
912			\|a GBV_ILN_171
912			\|a GBV_ILN_187
912			\|a GBV_ILN_213
912			\|a GBV_ILN_224
912			\|a GBV_ILN_230
912			\|a GBV_ILN_250
912			\|a GBV_ILN_281
912			\|a GBV_ILN_285
912			\|a GBV_ILN_293
912			\|a GBV_ILN_370
912			\|a GBV_ILN_602
912			\|a GBV_ILN_636
912			\|a GBV_ILN_702
912			\|a GBV_ILN_2001
912			\|a GBV_ILN_2003
912			\|a GBV_ILN_2004
912			\|a GBV_ILN_2005
912			\|a GBV_ILN_2006
912			\|a GBV_ILN_2007
912			\|a GBV_ILN_2008
912			\|a GBV_ILN_2009
912			\|a GBV_ILN_2010
912			\|a GBV_ILN_2011
912			\|a GBV_ILN_2014
912			\|a GBV_ILN_2015
912			\|a GBV_ILN_2020
912			\|a GBV_ILN_2021
912			\|a GBV_ILN_2025
912			\|a GBV_ILN_2026
912			\|a GBV_ILN_2027
912			\|a GBV_ILN_2031
912			\|a GBV_ILN_2034
912			\|a GBV_ILN_2037
912			\|a GBV_ILN_2038
912			\|a GBV_ILN_2039
912			\|a GBV_ILN_2044
912			\|a GBV_ILN_2048
912			\|a GBV_ILN_2049
912			\|a GBV_ILN_2050
912			\|a GBV_ILN_2055
912			\|a GBV_ILN_2057
912			\|a GBV_ILN_2059
912			\|a GBV_ILN_2061
912			\|a GBV_ILN_2064
912			\|a GBV_ILN_2065
912			\|a GBV_ILN_2068
912			\|a GBV_ILN_2070
912			\|a GBV_ILN_2086
912			\|a GBV_ILN_2088
912			\|a GBV_ILN_2093
912			\|a GBV_ILN_2106
912			\|a GBV_ILN_2107
912			\|a GBV_ILN_2108
912			\|a GBV_ILN_2110
912			\|a GBV_ILN_2111
912			\|a GBV_ILN_2112
912			\|a GBV_ILN_2113
912			\|a GBV_ILN_2116
912			\|a GBV_ILN_2118
912			\|a GBV_ILN_2119
912			\|a GBV_ILN_2122
912			\|a GBV_ILN_2129
912			\|a GBV_ILN_2143
912			\|a GBV_ILN_2144
912			\|a GBV_ILN_2147
912			\|a GBV_ILN_2148
912			\|a GBV_ILN_2152
912			\|a GBV_ILN_2153
912			\|a GBV_ILN_2188
912			\|a GBV_ILN_2190
912			\|a GBV_ILN_2232
912			\|a GBV_ILN_2336
912			\|a GBV_ILN_2446
912			\|a GBV_ILN_2470
912			\|a GBV_ILN_2472
912			\|a GBV_ILN_2507
912			\|a GBV_ILN_2522
912			\|a GBV_ILN_2548
912			\|a GBV_ILN_4035
912			\|a GBV_ILN_4037
912			\|a GBV_ILN_4046
912			\|a GBV_ILN_4112
912			\|a GBV_ILN_4125
912			\|a GBV_ILN_4242
912			\|a GBV_ILN_4246
912			\|a GBV_ILN_4249
912			\|a GBV_ILN_4251
912			\|a GBV_ILN_4305
912			\|a GBV_ILN_4306
912			\|a GBV_ILN_4307
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912			\|a GBV_ILN_4322
912			\|a GBV_ILN_4323
912			\|a GBV_ILN_4324
912			\|a GBV_ILN_4325
912			\|a GBV_ILN_4326
912			\|a GBV_ILN_4333
912			\|a GBV_ILN_4334
912			\|a GBV_ILN_4335
912			\|a GBV_ILN_4336
912			\|a GBV_ILN_4338
912			\|a GBV_ILN_4393
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951			\|a AR
952			\|d 55 \|j 2015 \|e 2 \|c 03 \|h 185-191

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author_variant	f z f fz fzf y g k yg ygk n g k ng ngk l m m lm lmm t r tr
matchkey_str	article:1555645X:2015----::hwdhfhfeunypcrmfcgoantcustosnue
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publishDate	2015
allfields	10.1134/S0016793215020048 doi (DE-627)SPR020000251 (SPR)S0016793215020048-e DE-627 ger DE-627 rakwb eng Feygin, F. Z. verfasserin aut The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere. Wave Packet (dpeaa)DE-He213 EMIC Wave (dpeaa)DE-He213 Energetic Proton (dpeaa)DE-He213 Narrow Frequency Band (dpeaa)DE-He213 Outer Radiation Belt (dpeaa)DE-He213 Khabazin, Yu. G. aut Kleimenova, N. G. aut Malysheva, L. M. aut Raita, T. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 185-191 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:185-191 https://dx.doi.org/10.1134/S0016793215020048 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 03 185-191
spelling	10.1134/S0016793215020048 doi (DE-627)SPR020000251 (SPR)S0016793215020048-e DE-627 ger DE-627 rakwb eng Feygin, F. Z. verfasserin aut The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere. Wave Packet (dpeaa)DE-He213 EMIC Wave (dpeaa)DE-He213 Energetic Proton (dpeaa)DE-He213 Narrow Frequency Band (dpeaa)DE-He213 Outer Radiation Belt (dpeaa)DE-He213 Khabazin, Yu. G. aut Kleimenova, N. G. aut Malysheva, L. M. aut Raita, T. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 185-191 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:185-191 https://dx.doi.org/10.1134/S0016793215020048 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 03 185-191
allfields_unstemmed	10.1134/S0016793215020048 doi (DE-627)SPR020000251 (SPR)S0016793215020048-e DE-627 ger DE-627 rakwb eng Feygin, F. Z. verfasserin aut The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere. Wave Packet (dpeaa)DE-He213 EMIC Wave (dpeaa)DE-He213 Energetic Proton (dpeaa)DE-He213 Narrow Frequency Band (dpeaa)DE-He213 Outer Radiation Belt (dpeaa)DE-He213 Khabazin, Yu. G. aut Kleimenova, N. G. aut Malysheva, L. M. aut Raita, T. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 185-191 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:185-191 https://dx.doi.org/10.1134/S0016793215020048 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 03 185-191
allfieldsGer	10.1134/S0016793215020048 doi (DE-627)SPR020000251 (SPR)S0016793215020048-e DE-627 ger DE-627 rakwb eng Feygin, F. Z. verfasserin aut The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere. Wave Packet (dpeaa)DE-He213 EMIC Wave (dpeaa)DE-He213 Energetic Proton (dpeaa)DE-He213 Narrow Frequency Band (dpeaa)DE-He213 Outer Radiation Belt (dpeaa)DE-He213 Khabazin, Yu. G. aut Kleimenova, N. G. aut Malysheva, L. M. aut Raita, T. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 185-191 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:185-191 https://dx.doi.org/10.1134/S0016793215020048 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 03 185-191
allfieldsSound	10.1134/S0016793215020048 doi (DE-627)SPR020000251 (SPR)S0016793215020048-e DE-627 ger DE-627 rakwb eng Feygin, F. Z. verfasserin aut The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions 2015 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Pleiades Publishing, Ltd. 2015 Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere. Wave Packet (dpeaa)DE-He213 EMIC Wave (dpeaa)DE-He213 Energetic Proton (dpeaa)DE-He213 Narrow Frequency Band (dpeaa)DE-He213 Outer Radiation Belt (dpeaa)DE-He213 Khabazin, Yu. G. aut Kleimenova, N. G. aut Malysheva, L. M. aut Raita, T. aut Enthalten in Geomagnetism and aeronomy Moscow : MAIK Nauka/Interperiodica Publ., 1996 55(2015), 2 vom: März, Seite 185-191 (DE-627)342320920 (DE-600)2071667-9 1555-645X nnns volume:55 year:2015 number:2 month:03 pages:185-191 https://dx.doi.org/10.1134/S0016793215020048 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 03 185-191
language	English
source	Enthalten in Geomagnetism and aeronomy 55(2015), 2 vom: März, Seite 185-191 volume:55 year:2015 number:2 month:03 pages:185-191
sourceStr	Enthalten in Geomagnetism and aeronomy 55(2015), 2 vom: März, Seite 185-191 volume:55 year:2015 number:2 month:03 pages:185-191
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Wave Packet EMIC Wave Energetic Proton Narrow Frequency Band Outer Radiation Belt
isfreeaccess_bool	false
container_title	Geomagnetism and aeronomy
authorswithroles_txt_mv	Feygin, F. Z. @@aut@@ Khabazin, Yu. G. @@aut@@ Kleimenova, N. G. @@aut@@ Malysheva, L. M. @@aut@@ Raita, T. @@aut@@
publishDateDaySort_date	2015-03-01T00:00:00Z
hierarchy_top_id	342320920
id	SPR020000251
language_de	englisch
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author	Feygin, F. Z.
spellingShingle	Feygin, F. Z. misc Wave Packet misc EMIC Wave misc Energetic Proton misc Narrow Frequency Band misc Outer Radiation Belt The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions
authorStr	Feygin, F. Z.
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topic_title	The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions Wave Packet (dpeaa)DE-He213 EMIC Wave (dpeaa)DE-He213 Energetic Proton (dpeaa)DE-He213 Narrow Frequency Band (dpeaa)DE-He213 Outer Radiation Belt (dpeaa)DE-He213
topic	misc Wave Packet misc EMIC Wave misc Energetic Proton misc Narrow Frequency Band misc Outer Radiation Belt
topic_unstemmed	misc Wave Packet misc EMIC Wave misc Energetic Proton misc Narrow Frequency Band misc Outer Radiation Belt
topic_browse	misc Wave Packet misc EMIC Wave misc Energetic Proton misc Narrow Frequency Band misc Outer Radiation Belt
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title	The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions
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title_full	The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions
author_sort	Feygin, F. Z.
journal	Geomagnetism and aeronomy
journalStr	Geomagnetism and aeronomy
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author_browse	Feygin, F. Z. Khabazin, Yu. G. Kleimenova, N. G. Malysheva, L. M. Raita, T.
container_volume	55
format_se	Elektronische Aufsätze
author-letter	Feygin, F. Z.
doi_str_mv	10.1134/S0016793215020048
title_sort	width of the frequency spectrum of pc1 geomagnetic pulsations in quiet and disturbed conditions
title_auth	The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions
abstract	Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere. © Pleiades Publishing, Ltd. 2015
abstractGer	Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere. © Pleiades Publishing, Ltd. 2015
abstract_unstemmed	Abstract The relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere. © Pleiades Publishing, Ltd. 2015
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title_short	The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions
url	https://dx.doi.org/10.1134/S0016793215020048
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author2	Khabazin, Yu. G. Kleimenova, N. G. Malysheva, L. M. Raita, T.
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up_date	2024-07-04T03:36:33.195Z
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fullrecord_marcxml	<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">SPR020000251</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230330160707.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">201006s2015 xx \|\|\|\|\|o 00\| \|\|eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1134/S0016793215020048</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)SPR020000251</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(SPR)S0016793215020048-e</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Feygin, F. Z.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="4"><subfield code="a">The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions</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 relation of the frequency spectrum width of Pc1 geomagnetic pulsations with magnetospheric parameters was theoretically studied. An analytical expression was obtained and numerical calculations were conducted. The formula for the increment (γ) was shown to include an important magnetospheric parameter, the ratio (VA/U‖) of the Alfven velocity to the average velocity of energetic protons along the field line, which significantly affects the frequency spectrum width. The calculations show that the normalized width of the Pc1 frequency spectrum (x0 = $ ω_{out} $/$ Ω_{i} $ = VA/U‖) decreases with decreasing (VA/U‖). With increasing anisotropy of energetic protons A = T⊥/T‖ − 1, the normalized width of Pc1 frequency spectrum is also decreased for a fixed value of the parameter (VA/U‖). These conclusions have been confirmed by analysis of spectrograms conducted in 2005–2010 of ground-based observations of Pc1 on the Scandinavian network of induction magnetometers. Analysis of these data showed that Pc1 pulsations were observed in a narrow frequency band of around 0.2–0.4 Hz, with a central frequency of oscillations in the series f ∼ 0.5–0.7 Hz, in more than 90% of cases in magnetically quiet conditions (Kp < 2). This corresponds to their generation beyond the plasmasphere. In more disturbed conditions (Kp ∼ 2–3), the central frequency of Pc1 oscillations was almost twice greater (∼ 1.0–1.2 Hz) and the spectral width was ∼ 0.5–0.7 Hz, which makes it possible to suggest that they can be generated within the plasmasphere.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Wave Packet</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">EMIC Wave</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Energetic Proton</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Narrow Frequency Band</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Outer Radiation Belt</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Khabazin, Yu. G.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Kleimenova, N. G.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Malysheva, L. M.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Raita, T.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Geomagnetism and aeronomy</subfield><subfield code="d">Moscow : MAIK Nauka/Interperiodica Publ., 1996</subfield><subfield code="g">55(2015), 2 vom: März, Seite 185-191</subfield><subfield code="w">(DE-627)342320920</subfield><subfield code="w">(DE-600)2071667-9</subfield><subfield code="x">1555-645X</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:55</subfield><subfield code="g">year:2015</subfield><subfield code="g">number:2</subfield><subfield code="g">month:03</subfield><subfield code="g">pages:185-191</subfield></datafield><datafield tag="856" ind1="4" ind2="0"><subfield 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The width of the frequency spectrum of Pc1 geomagnetic pulsations in quiet and disturbed conditions

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