Decameter U-burst Harmonic Pair from a High Loop
Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Dorovskyy, V. V. [verfasserIn] Melnik, V. N. [verfasserIn] Konovalenko, A. A. [verfasserIn] Bubnov, I. N. [verfasserIn] Gridin, A. A. [verfasserIn] Shevchuk, N. V. [verfasserIn] Rucker, H. O. [verfasserIn] Poedts, S. [verfasserIn] Panchenko, M. [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2014 |
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| Schlagwörter: |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967, 290(2014), 1 vom: 21. Okt., Seite 181-192 |
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| Übergeordnetes Werk: |
volume:290 ; year:2014 ; number:1 ; day:21 ; month:10 ; pages:181-192 |
| Links: |
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| DOI / URN: |
10.1007/s11207-014-0615-6 |
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| Katalog-ID: |
SPR017766923 |
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| 520 | |a Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. | ||
| 650 | 4 | |a Corona, radio emission |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Corona, structures |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 U |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Radio bursts, harmonic pairs |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Melnik, V. N. |e verfasserin |4 aut | |
| 700 | 1 | |a Konovalenko, A. A. |e verfasserin |4 aut | |
| 700 | 1 | |a Bubnov, I. N. |e verfasserin |4 aut | |
| 700 | 1 | |a Gridin, A. A. |e verfasserin |4 aut | |
| 700 | 1 | |a Shevchuk, N. V. |e verfasserin |4 aut | |
| 700 | 1 | |a Rucker, H. O. |e verfasserin |4 aut | |
| 700 | 1 | |a Poedts, S. |e verfasserin |4 aut | |
| 700 | 1 | |a Panchenko, M. |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 290(2014), 1 vom: 21. Okt., Seite 181-192 |w (DE-627)269019162 |w (DE-600)1473830-2 |x 1573-093X |7 nnns |
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10.1007/s11207-014-0615-6 doi (DE-627)SPR017766923 (SPR)s11207-014-0615-6-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Dorovskyy, V. V. verfasserin aut Decameter U-burst Harmonic Pair from a High Loop 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. Corona, radio emission (dpeaa)DE-He213 Corona, structures (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type U (dpeaa)DE-He213 Radio bursts, harmonic pairs (dpeaa)DE-He213 Melnik, V. N. verfasserin aut Konovalenko, A. A. verfasserin aut Bubnov, I. N. verfasserin aut Gridin, A. A. verfasserin aut Shevchuk, N. V. verfasserin aut Rucker, H. O. verfasserin aut Poedts, S. verfasserin aut Panchenko, M. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 290(2014), 1 vom: 21. Okt., Seite 181-192 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:290 year:2014 number:1 day:21 month:10 pages:181-192 https://dx.doi.org/10.1007/s11207-014-0615-6 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 290 2014 1 21 10 181-192 |
| spelling |
10.1007/s11207-014-0615-6 doi (DE-627)SPR017766923 (SPR)s11207-014-0615-6-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Dorovskyy, V. V. verfasserin aut Decameter U-burst Harmonic Pair from a High Loop 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. Corona, radio emission (dpeaa)DE-He213 Corona, structures (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type U (dpeaa)DE-He213 Radio bursts, harmonic pairs (dpeaa)DE-He213 Melnik, V. N. verfasserin aut Konovalenko, A. A. verfasserin aut Bubnov, I. N. verfasserin aut Gridin, A. A. verfasserin aut Shevchuk, N. V. verfasserin aut Rucker, H. O. verfasserin aut Poedts, S. verfasserin aut Panchenko, M. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 290(2014), 1 vom: 21. Okt., Seite 181-192 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:290 year:2014 number:1 day:21 month:10 pages:181-192 https://dx.doi.org/10.1007/s11207-014-0615-6 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 290 2014 1 21 10 181-192 |
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10.1007/s11207-014-0615-6 doi (DE-627)SPR017766923 (SPR)s11207-014-0615-6-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Dorovskyy, V. V. verfasserin aut Decameter U-burst Harmonic Pair from a High Loop 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. Corona, radio emission (dpeaa)DE-He213 Corona, structures (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type U (dpeaa)DE-He213 Radio bursts, harmonic pairs (dpeaa)DE-He213 Melnik, V. N. verfasserin aut Konovalenko, A. A. verfasserin aut Bubnov, I. N. verfasserin aut Gridin, A. A. verfasserin aut Shevchuk, N. V. verfasserin aut Rucker, H. O. verfasserin aut Poedts, S. verfasserin aut Panchenko, M. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 290(2014), 1 vom: 21. Okt., Seite 181-192 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:290 year:2014 number:1 day:21 month:10 pages:181-192 https://dx.doi.org/10.1007/s11207-014-0615-6 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 290 2014 1 21 10 181-192 |
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10.1007/s11207-014-0615-6 doi (DE-627)SPR017766923 (SPR)s11207-014-0615-6-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Dorovskyy, V. V. verfasserin aut Decameter U-burst Harmonic Pair from a High Loop 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. Corona, radio emission (dpeaa)DE-He213 Corona, structures (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type U (dpeaa)DE-He213 Radio bursts, harmonic pairs (dpeaa)DE-He213 Melnik, V. N. verfasserin aut Konovalenko, A. A. verfasserin aut Bubnov, I. N. verfasserin aut Gridin, A. A. verfasserin aut Shevchuk, N. V. verfasserin aut Rucker, H. O. verfasserin aut Poedts, S. verfasserin aut Panchenko, M. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 290(2014), 1 vom: 21. Okt., Seite 181-192 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:290 year:2014 number:1 day:21 month:10 pages:181-192 https://dx.doi.org/10.1007/s11207-014-0615-6 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 290 2014 1 21 10 181-192 |
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10.1007/s11207-014-0615-6 doi (DE-627)SPR017766923 (SPR)s11207-014-0615-6-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Dorovskyy, V. V. verfasserin aut Decameter U-burst Harmonic Pair from a High Loop 2014 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. Corona, radio emission (dpeaa)DE-He213 Corona, structures (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type U (dpeaa)DE-He213 Radio bursts, harmonic pairs (dpeaa)DE-He213 Melnik, V. N. verfasserin aut Konovalenko, A. A. verfasserin aut Bubnov, I. N. verfasserin aut Gridin, A. A. verfasserin aut Shevchuk, N. V. verfasserin aut Rucker, H. O. verfasserin aut Poedts, S. verfasserin aut Panchenko, M. verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 290(2014), 1 vom: 21. Okt., Seite 181-192 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:290 year:2014 number:1 day:21 month:10 pages:181-192 https://dx.doi.org/10.1007/s11207-014-0615-6 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 290 2014 1 21 10 181-192 |
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Enthalten in Solar physics 290(2014), 1 vom: 21. Okt., Seite 181-192 volume:290 year:2014 number:1 day:21 month:10 pages:181-192 |
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Enthalten in Solar physics 290(2014), 1 vom: 21. Okt., Seite 181-192 volume:290 year:2014 number:1 day:21 month:10 pages:181-192 |
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Corona, radio emission Corona, structures Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) Radio bursts, type U Radio bursts, harmonic pairs |
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Dorovskyy, V. V. @@aut@@ Melnik, V. N. @@aut@@ Konovalenko, A. A. @@aut@@ Bubnov, I. N. @@aut@@ Gridin, A. A. @@aut@@ Shevchuk, N. V. @@aut@@ Rucker, H. O. @@aut@@ Poedts, S. @@aut@@ Panchenko, M. @@aut@@ |
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V.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Decameter U-burst Harmonic Pair from a High Loop</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2014</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 The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Corona, radio emission</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Corona, structures</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 U</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Radio bursts, harmonic pairs</subfield><subfield code="7">(dpeaa)DE-He213</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Melnik, V. 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Dorovskyy, V. V. |
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530 ASE 39.51 bkl Decameter U-burst Harmonic Pair from a High Loop Corona, radio emission (dpeaa)DE-He213 Corona, structures (dpeaa)DE-He213 Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) (dpeaa)DE-He213 Radio bursts, type U (dpeaa)DE-He213 Radio bursts, harmonic pairs (dpeaa)DE-He213 |
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ddc 530 bkl 39.51 misc Corona, radio emission misc Corona, structures misc Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) misc Radio bursts, type U misc Radio bursts, harmonic pairs |
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ddc 530 bkl 39.51 misc Corona, radio emission misc Corona, structures misc Radio bursts, meter-wavelengths and longer (m, dkm, hm, km) misc Radio bursts, type U misc Radio bursts, harmonic pairs |
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Decameter U-burst Harmonic Pair from a High Loop |
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Dorovskyy, V. V. Melnik, V. N. Konovalenko, A. A. Bubnov, I. N. Gridin, A. A. Shevchuk, N. V. Rucker, H. O. Poedts, S. Panchenko, M. |
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decameter u-burst harmonic pair from a high loop |
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Decameter U-burst Harmonic Pair from a High Loop |
| abstract |
Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. |
| abstractGer |
Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. |
| abstract_unstemmed |
Abstract The results of the first observations of solar sporadic radio emission within 10 – 70 MHz by the Giant Ukrainian Radio Telescope (GURT) are presented and discussed. Observations in such a wide range of frequencies considerably facilitate the registration of harmonic pairs. The solar U-burst harmonic pair observed on 8 August 2012 is analyzed. The burst key features were determined. Among them, the time delay between the fundamental and harmonic emissions was of special interest. The fundamental emission was delayed for 7 s with respect to the harmonic emission. A model for explaining the occurrence of such a delay is proposed, in which the emission source is located inside a magnetic loop containing plasma of increased density. In this case, the delay appears due to the difference in group velocities of electromagnetic waves at the fundamental and the harmonic frequencies. |
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| title_short |
Decameter U-burst Harmonic Pair from a High Loop |
| url |
https://dx.doi.org/10.1007/s11207-014-0615-6 |
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true |
| author2 |
Melnik, V. N. Konovalenko, A. A. Bubnov, I. N. Gridin, A. A. Shevchuk, N. V. Rucker, H. O. Poedts, S. Panchenko, M. |
| author2Str |
Melnik, V. N. Konovalenko, A. A. Bubnov, I. N. Gridin, A. A. Shevchuk, N. V. Rucker, H. O. Poedts, S. Panchenko, M. |
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| doi_str |
10.1007/s11207-014-0615-6 |
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2024-07-03T15:04:15.907Z |
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1803570701575127040 |
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| score |
7.4011803 |