Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing

Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made...
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Gespeichert in:

Autor*in:	Chelpanov, A. A. [verfasserIn] Kobanov, N. I. [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2020

Übergeordnetes Werk:	Enthalten in: Astronomy reports - Moscow : MAIK Nauka/Interperiodika, 1993, 64(2020), 4 vom: Apr., Seite 363-368
Übergeordnetes Werk:	volume:64 ; year:2020 ; number:4 ; month:04 ; pages:363-368

Links:	Volltext

DOI / URN:	10.1134/S1063772920030026

Katalog-ID:	SPR039396169

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520			\|a Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere.
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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_206
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_647
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_2056
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_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_2118
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_4126
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
912			\|a GBV_ILN_4313
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_4328
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
912			\|a GBV_ILN_4700
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author_variant	a a c aa aac n i k ni nik
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allfields	10.1134/S1063772920030026 doi (DE-627)SPR039396169 (SPR)S1063772920030026-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Chelpanov, A. A. verfasserin aut Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere. Kobanov, N. I. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 64(2020), 4 vom: Apr., Seite 363-368 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:64 year:2020 number:4 month:04 pages:363-368 https://dx.doi.org/10.1134/S1063772920030026 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE 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_206 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_647 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_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 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_2118 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_4126 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_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 64 2020 4 04 363-368
spelling	10.1134/S1063772920030026 doi (DE-627)SPR039396169 (SPR)S1063772920030026-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Chelpanov, A. A. verfasserin aut Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere. Kobanov, N. I. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 64(2020), 4 vom: Apr., Seite 363-368 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:64 year:2020 number:4 month:04 pages:363-368 https://dx.doi.org/10.1134/S1063772920030026 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE 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_206 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_647 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_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 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_2118 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_4126 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_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 64 2020 4 04 363-368
allfields_unstemmed	10.1134/S1063772920030026 doi (DE-627)SPR039396169 (SPR)S1063772920030026-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Chelpanov, A. A. verfasserin aut Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere. Kobanov, N. I. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 64(2020), 4 vom: Apr., Seite 363-368 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:64 year:2020 number:4 month:04 pages:363-368 https://dx.doi.org/10.1134/S1063772920030026 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE 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_206 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_647 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_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 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_2118 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_4126 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_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 64 2020 4 04 363-368
allfieldsGer	10.1134/S1063772920030026 doi (DE-627)SPR039396169 (SPR)S1063772920030026-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Chelpanov, A. A. verfasserin aut Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere. Kobanov, N. I. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 64(2020), 4 vom: Apr., Seite 363-368 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:64 year:2020 number:4 month:04 pages:363-368 https://dx.doi.org/10.1134/S1063772920030026 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE 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_206 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_647 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_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 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_2118 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_4126 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_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 64 2020 4 04 363-368
allfieldsSound	10.1134/S1063772920030026 doi (DE-627)SPR039396169 (SPR)S1063772920030026-e DE-627 ger DE-627 rakwb eng 520 ASE 39.00 bkl Chelpanov, A. A. verfasserin aut Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere. Kobanov, N. I. verfasserin aut Enthalten in Astronomy reports Moscow : MAIK Nauka/Interperiodika, 1993 64(2020), 4 vom: Apr., Seite 363-368 (DE-627)312182287 (DE-600)2010316-5 1562-6881 nnns volume:64 year:2020 number:4 month:04 pages:363-368 https://dx.doi.org/10.1134/S1063772920030026 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE 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_206 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_647 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_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 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_2118 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_4126 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_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.00 ASE AR 64 2020 4 04 363-368
language	English
source	Enthalten in Astronomy reports 64(2020), 4 vom: Apr., Seite 363-368 volume:64 year:2020 number:4 month:04 pages:363-368
sourceStr	Enthalten in Astronomy reports 64(2020), 4 vom: Apr., Seite 363-368 volume:64 year:2020 number:4 month:04 pages:363-368
format_phy_str_mv	Article
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container_title	Astronomy reports
authorswithroles_txt_mv	Chelpanov, A. A. @@aut@@ Kobanov, N. I. @@aut@@
publishDateDaySort_date	2020-04-01T00:00:00Z
hierarchy_top_id	312182287
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author	Chelpanov, A. A.
spellingShingle	Chelpanov, A. A. ddc 520 bkl 39.00 Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing
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topic_title	520 ASE 39.00 bkl Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing
topic	ddc 520 bkl 39.00
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title	Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing
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title_full	Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing
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journal	Astronomy reports
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author_browse	Chelpanov, A. A. Kobanov, N. I.
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author-letter	Chelpanov, A. A.
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title_sort	three- and five-minute oscillations modulated by flares as a means of solar atmosphere sensing
title_auth	Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing
abstract	Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere.
abstractGer	Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere.
abstract_unstemmed	Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. A small flare in the flare region of the chromosphere served as a modulator of 3‑ and 5-minute oscillations. The oscillation amplitude increased several times, which made it possible to easily fix the wave train formed as it spread upward through the solar atmosphere layers. Such a short-term and well-defined wave train serves as a convenient tool for determining the velocity of propagating magnetohydrodynamic waves, since it avoids the uncertainties in the measurement of the phase shift that arise under ordinary conditions. The advantage of using amplitude modulation from a small flare is that it makes it possible to study the atmosphere of the Sun under conditions close to those in an unperturbed atmosphere.
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container_issue	4
title_short	Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing
url	https://dx.doi.org/10.1134/S1063772920030026
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author2	Kobanov, N. I.
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doi_str	10.1134/S1063772920030026
up_date	2024-07-03T23:43:38.699Z
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A.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2020</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract— We applied a new approach to measure the time delays of magnetohydrodynamic waves propagating in the solar atmosphere. 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Three- and Five-Minute Oscillations Modulated by Flares as a Means of Solar Atmosphere Sensing

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