Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013
Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) an...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Melnik, V. N. [verfasserIn] Brazhenko, A. I. [verfasserIn] Konovalenko, A. A. [verfasserIn] Dorovskyy, V. V. [verfasserIn] Rucker, H. O. [verfasserIn] Panchenko, M. [verfasserIn] Frantsuzenko, A. V. [verfasserIn] Shevchuk, M. V. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2018 |
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| Schlagwörter: |
Coronal mass ejections, initiation and propagation |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967, 293(2018), 3 vom: 13. März |
|---|---|
| Übergeordnetes Werk: |
volume:293 ; year:2018 ; number:3 ; day:13 ; month:03 |
| Links: |
|---|
| DOI / URN: |
10.1007/s11207-018-1271-z |
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| Katalog-ID: |
SPR017774438 |
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| 520 | |a Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. | ||
| 650 | 4 | |a Coronal mass ejections, initiation and propagation |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Radio bursts, type II |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Radio bursts, type III |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Radio bursts, type IV |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Brazhenko, A. I. |e verfasserin |4 aut | |
| 700 | 1 | |a Konovalenko, A. A. |e verfasserin |4 aut | |
| 700 | 1 | |a Dorovskyy, V. V. |e verfasserin |4 aut | |
| 700 | 1 | |a Rucker, H. O. |e verfasserin |4 aut | |
| 700 | 1 | |a Panchenko, M. |e verfasserin |4 aut | |
| 700 | 1 | |a Frantsuzenko, A. V. |e verfasserin |4 aut | |
| 700 | 1 | |a Shevchuk, M. V. |e verfasserin |4 aut | |
| 773 | 0 | 8 | |i Enthalten in |t Solar physics |d Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 |g 293(2018), 3 vom: 13. März |w (DE-627)269019162 |w (DE-600)1473830-2 |x 1573-093X |7 nnns |
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10.1007/s11207-018-1271-z doi (DE-627)SPR017774438 (SPR)s11207-018-1271-z-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Melnik, V. N. verfasserin aut Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. Coronal mass ejections, initiation and propagation (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type II (dpeaa)DE-He213 Radio bursts, type III (dpeaa)DE-He213 Radio bursts, type IV (dpeaa)DE-He213 Brazhenko, A. I. verfasserin aut Konovalenko, A. A. verfasserin aut Dorovskyy, V. V. verfasserin aut Rucker, H. O. verfasserin aut Panchenko, M. verfasserin aut Frantsuzenko, A. V. verfasserin aut Shevchuk, M. V. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 293(2018), 3 vom: 13. März (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:293 year:2018 number:3 day:13 month:03 https://dx.doi.org/10.1007/s11207-018-1271-z 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_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 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_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_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 39.51 ASE AR 293 2018 3 13 03 |
| spelling |
10.1007/s11207-018-1271-z doi (DE-627)SPR017774438 (SPR)s11207-018-1271-z-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Melnik, V. N. verfasserin aut Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. Coronal mass ejections, initiation and propagation (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type II (dpeaa)DE-He213 Radio bursts, type III (dpeaa)DE-He213 Radio bursts, type IV (dpeaa)DE-He213 Brazhenko, A. I. verfasserin aut Konovalenko, A. A. verfasserin aut Dorovskyy, V. V. verfasserin aut Rucker, H. O. verfasserin aut Panchenko, M. verfasserin aut Frantsuzenko, A. V. verfasserin aut Shevchuk, M. V. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 293(2018), 3 vom: 13. März (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:293 year:2018 number:3 day:13 month:03 https://dx.doi.org/10.1007/s11207-018-1271-z 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_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 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_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_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 39.51 ASE AR 293 2018 3 13 03 |
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10.1007/s11207-018-1271-z doi (DE-627)SPR017774438 (SPR)s11207-018-1271-z-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Melnik, V. N. verfasserin aut Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. Coronal mass ejections, initiation and propagation (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type II (dpeaa)DE-He213 Radio bursts, type III (dpeaa)DE-He213 Radio bursts, type IV (dpeaa)DE-He213 Brazhenko, A. I. verfasserin aut Konovalenko, A. A. verfasserin aut Dorovskyy, V. V. verfasserin aut Rucker, H. O. verfasserin aut Panchenko, M. verfasserin aut Frantsuzenko, A. V. verfasserin aut Shevchuk, M. V. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 293(2018), 3 vom: 13. März (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:293 year:2018 number:3 day:13 month:03 https://dx.doi.org/10.1007/s11207-018-1271-z 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_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 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_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_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 39.51 ASE AR 293 2018 3 13 03 |
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10.1007/s11207-018-1271-z doi (DE-627)SPR017774438 (SPR)s11207-018-1271-z-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Melnik, V. N. verfasserin aut Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. Coronal mass ejections, initiation and propagation (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type II (dpeaa)DE-He213 Radio bursts, type III (dpeaa)DE-He213 Radio bursts, type IV (dpeaa)DE-He213 Brazhenko, A. I. verfasserin aut Konovalenko, A. A. verfasserin aut Dorovskyy, V. V. verfasserin aut Rucker, H. O. verfasserin aut Panchenko, M. verfasserin aut Frantsuzenko, A. V. verfasserin aut Shevchuk, M. V. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 293(2018), 3 vom: 13. März (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:293 year:2018 number:3 day:13 month:03 https://dx.doi.org/10.1007/s11207-018-1271-z 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_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 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_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_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 39.51 ASE AR 293 2018 3 13 03 |
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10.1007/s11207-018-1271-z doi (DE-627)SPR017774438 (SPR)s11207-018-1271-z-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Melnik, V. N. verfasserin aut Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 2018 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. Coronal mass ejections, initiation and propagation (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type II (dpeaa)DE-He213 Radio bursts, type III (dpeaa)DE-He213 Radio bursts, type IV (dpeaa)DE-He213 Brazhenko, A. I. verfasserin aut Konovalenko, A. A. verfasserin aut Dorovskyy, V. V. verfasserin aut Rucker, H. O. verfasserin aut Panchenko, M. verfasserin aut Frantsuzenko, A. V. verfasserin aut Shevchuk, M. V. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 293(2018), 3 vom: 13. März (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:293 year:2018 number:3 day:13 month:03 https://dx.doi.org/10.1007/s11207-018-1271-z 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_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 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_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_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 39.51 ASE AR 293 2018 3 13 03 |
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English |
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Enthalten in Solar physics 293(2018), 3 vom: 13. März volume:293 year:2018 number:3 day:13 month:03 |
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Enthalten in Solar physics 293(2018), 3 vom: 13. März volume:293 year:2018 number:3 day:13 month:03 |
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findex.gbv.de |
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Coronal mass ejections, initiation and propagation Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) Radio bursts, type II Radio bursts, type III Radio bursts, type IV |
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Melnik, V. N. @@aut@@ Brazhenko, A. I. @@aut@@ Konovalenko, A. A. @@aut@@ Dorovskyy, V. V. @@aut@@ Rucker, H. O. @@aut@@ Panchenko, M. @@aut@@ Frantsuzenko, A. V. @@aut@@ Shevchuk, M. V. @@aut@@ |
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2018-03-13T00:00:00Z |
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<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">SPR017774438</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20220111053602.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">201006s2018 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1007/s11207-018-1271-z</subfield><subfield code="2">doi</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)SPR017774438</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(SPR)s11207-018-1271-z-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="082" ind1="0" ind2="4"><subfield code="a">530</subfield><subfield code="q">ASE</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">39.51</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Melnik, V. N.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2018</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 report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Coronal mass ejections, initiation and propagation</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Radio bursts, meter-wavelengths and longer (m, dkm, hm, km)</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Radio bursts, type II</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Radio bursts, type III</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Radio bursts, type IV</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Brazhenko, A. 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V.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Shevchuk, M. V.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">Solar physics</subfield><subfield code="d">Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967</subfield><subfield code="g">293(2018), 3 vom: 13. 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|
| author |
Melnik, V. N. |
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Melnik, V. N. ddc 530 bkl 39.51 misc Coronal mass ejections, initiation and propagation misc Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) misc Radio bursts, type II misc Radio bursts, type III misc Radio bursts, type IV Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 |
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530 ASE 39.51 bkl Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 Coronal mass ejections, initiation and propagation (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type II (dpeaa)DE-He213 Radio bursts, type III (dpeaa)DE-He213 Radio bursts, type IV (dpeaa)DE-He213 |
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ddc 530 bkl 39.51 misc Coronal mass ejections, initiation and propagation misc Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) misc Radio bursts, type II misc Radio bursts, type III misc Radio bursts, type IV |
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ddc 530 bkl 39.51 misc Coronal mass ejections, initiation and propagation misc Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) misc Radio bursts, type II misc Radio bursts, type III misc Radio bursts, type IV |
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ddc 530 bkl 39.51 misc Coronal mass ejections, initiation and propagation misc Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) misc Radio bursts, type II misc Radio bursts, type III misc Radio bursts, type IV |
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Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 |
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Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 |
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Melnik, V. N. |
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Solar physics |
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Solar physics |
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eng |
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Melnik, V. N. Brazhenko, A. I. Konovalenko, A. A. Dorovskyy, V. V. Rucker, H. O. Panchenko, M. Frantsuzenko, A. V. Shevchuk, M. V. |
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Elektronische Aufsätze |
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Melnik, V. N. |
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10.1007/s11207-018-1271-z |
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decameter type iv burst associated with a behind-the-limb cme observed on 7 november 2013 |
| title_auth |
Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 |
| abstract |
Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. |
| abstractGer |
Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. |
| abstract_unstemmed |
Abstract We report on the results of observations of a type IV burst made by the Ukrainian Radio interferometer of the Academy of Sciences (URAN-2) in the frequency range 22 – 33 MHz. The burst is associated with a coronal mass ejection (CME) initiated by a behind-the-limb active region (N05E151) and was also observed by the Nançay Decameter Array (NDA) radio telescope in the frequency band 30 – 60 MHz. The purpose of the article is the determination of the source of this type IV burst. After analysis of the observational data obtained with the URAN-2, the NDA, the Solar-Terrestrial Relations Observatory (STEREO) A and B spacecraft, and the Solar and Heliospheric Observatory (SOHO) spacecraft, we come to the conclusion that the source of the burst is the core of a behind-the-limb CME. We conclude that the radio emission can escape the center of the CME core at a frequency of 60 MHz and originates from the periphery of the core at a frequency of 30 MHz that is due to occultation by the solar corona at the corresponding frequencies. We find plasma densities in these regions assuming the plasma mechanism of radio emission. We show that the frequency drift of the start of the type IV burst is governed by an expansion of the CME core. The type III bursts that were observed against this type IV burst are shown to be generated by fast electrons propagating through the CME core plasma. A type II burst was registered at frequencies of 44 – 64 MHz and 3 – 16 MHz and was radiated by a shock with velocities of about $1000~\mbox{km}\,\mbox{s}^{-1}$ and $800~\mbox{km}\,\mbox{s}^{-1}$, respectively. |
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3 |
| title_short |
Decameter Type IV Burst Associated with a Behind-the-limb CME Observed on 7 November 2013 |
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Brazhenko, A. I. Konovalenko, A. A. Dorovskyy, V. V. Rucker, H. O. Panchenko, M. Frantsuzenko, A. V. Shevchuk, M. V. |
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Brazhenko, A. I. Konovalenko, A. A. Dorovskyy, V. V. Rucker, H. O. Panchenko, M. Frantsuzenko, A. V. Shevchuk, M. V. |
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| score |
7.4007816 |