Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction
Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observa...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Huang, Guangli [verfasserIn] |
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| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2005 |
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| Schlagwörter: |
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| Anmerkung: |
© Springer Science + Business Media, Inc. 2005 |
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| Übergeordnetes Werk: |
Enthalten in: Solar physics - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967, 229(2005), 2 vom: 01. Juli, Seite 227-236 |
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| Übergeordnetes Werk: |
volume:229 ; year:2005 ; number:2 ; day:01 ; month:07 ; pages:227-236 |
| Links: |
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| DOI / URN: |
10.1007/s11207-005-7448-2 |
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| Katalog-ID: |
SPR054851890 |
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| 520 | |a Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. | ||
| 650 | 4 | |a Flare |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Light Curve |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Coronal Loop |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Spectroscopic Imager |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Ramaty High Energy Solar Spectroscopic Imager |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Ji, Haisheng |4 aut | |
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10.1007/s11207-005-7448-2 doi (DE-627)SPR054851890 (SPR)s11207-005-7448-2-e DE-627 ger DE-627 rakwb eng Huang, Guangli verfasserin aut Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Springer Science + Business Media, Inc. 2005 Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. Flare (dpeaa)DE-He213 Light Curve (dpeaa)DE-He213 Coronal Loop (dpeaa)DE-He213 Spectroscopic Imager (dpeaa)DE-He213 Ramaty High Energy Solar Spectroscopic Imager (dpeaa)DE-He213 Ji, Haisheng aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 229(2005), 2 vom: 01. Juli, Seite 227-236 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:229 year:2005 number:2 day:01 month:07 pages:227-236 https://dx.doi.org/10.1007/s11207-005-7448-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_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 AR 229 2005 2 01 07 227-236 |
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10.1007/s11207-005-7448-2 doi (DE-627)SPR054851890 (SPR)s11207-005-7448-2-e DE-627 ger DE-627 rakwb eng Huang, Guangli verfasserin aut Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Springer Science + Business Media, Inc. 2005 Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. Flare (dpeaa)DE-He213 Light Curve (dpeaa)DE-He213 Coronal Loop (dpeaa)DE-He213 Spectroscopic Imager (dpeaa)DE-He213 Ramaty High Energy Solar Spectroscopic Imager (dpeaa)DE-He213 Ji, Haisheng aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 229(2005), 2 vom: 01. Juli, Seite 227-236 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:229 year:2005 number:2 day:01 month:07 pages:227-236 https://dx.doi.org/10.1007/s11207-005-7448-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_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 AR 229 2005 2 01 07 227-236 |
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10.1007/s11207-005-7448-2 doi (DE-627)SPR054851890 (SPR)s11207-005-7448-2-e DE-627 ger DE-627 rakwb eng Huang, Guangli verfasserin aut Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Springer Science + Business Media, Inc. 2005 Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. Flare (dpeaa)DE-He213 Light Curve (dpeaa)DE-He213 Coronal Loop (dpeaa)DE-He213 Spectroscopic Imager (dpeaa)DE-He213 Ramaty High Energy Solar Spectroscopic Imager (dpeaa)DE-He213 Ji, Haisheng aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 229(2005), 2 vom: 01. Juli, Seite 227-236 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:229 year:2005 number:2 day:01 month:07 pages:227-236 https://dx.doi.org/10.1007/s11207-005-7448-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_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 AR 229 2005 2 01 07 227-236 |
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10.1007/s11207-005-7448-2 doi (DE-627)SPR054851890 (SPR)s11207-005-7448-2-e DE-627 ger DE-627 rakwb eng Huang, Guangli verfasserin aut Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Springer Science + Business Media, Inc. 2005 Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. Flare (dpeaa)DE-He213 Light Curve (dpeaa)DE-He213 Coronal Loop (dpeaa)DE-He213 Spectroscopic Imager (dpeaa)DE-He213 Ramaty High Energy Solar Spectroscopic Imager (dpeaa)DE-He213 Ji, Haisheng aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 229(2005), 2 vom: 01. Juli, Seite 227-236 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:229 year:2005 number:2 day:01 month:07 pages:227-236 https://dx.doi.org/10.1007/s11207-005-7448-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_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 AR 229 2005 2 01 07 227-236 |
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10.1007/s11207-005-7448-2 doi (DE-627)SPR054851890 (SPR)s11207-005-7448-2-e DE-627 ger DE-627 rakwb eng Huang, Guangli verfasserin aut Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction 2005 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier © Springer Science + Business Media, Inc. 2005 Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. Flare (dpeaa)DE-He213 Light Curve (dpeaa)DE-He213 Coronal Loop (dpeaa)DE-He213 Spectroscopic Imager (dpeaa)DE-He213 Ramaty High Energy Solar Spectroscopic Imager (dpeaa)DE-He213 Ji, Haisheng aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 229(2005), 2 vom: 01. Juli, Seite 227-236 (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:229 year:2005 number:2 day:01 month:07 pages:227-236 https://dx.doi.org/10.1007/s11207-005-7448-2 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_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 AR 229 2005 2 01 07 227-236 |
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Enthalten in Solar physics 229(2005), 2 vom: 01. Juli, Seite 227-236 volume:229 year:2005 number:2 day:01 month:07 pages:227-236 |
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Enthalten in Solar physics 229(2005), 2 vom: 01. Juli, Seite 227-236 volume:229 year:2005 number:2 day:01 month:07 pages:227-236 |
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The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. 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| author |
Huang, Guangli |
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Huang, Guangli misc Flare misc Light Curve misc Coronal Loop misc Spectroscopic Imager misc Ramaty High Energy Solar Spectroscopic Imager Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction |
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Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction Flare (dpeaa)DE-He213 Light Curve (dpeaa)DE-He213 Coronal Loop (dpeaa)DE-He213 Spectroscopic Imager (dpeaa)DE-He213 Ramaty High Energy Solar Spectroscopic Imager (dpeaa)DE-He213 |
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Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction |
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Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction |
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microwave, optical, euv, and hard x-ray signature of possible coronal loop interaction |
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Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction |
| abstract |
Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. © Springer Science + Business Media, Inc. 2005 |
| abstractGer |
Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. © Springer Science + Business Media, Inc. 2005 |
| abstract_unstemmed |
Abstract In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of $ H_{α} $ − 1.3 Å with a cadence of ∼40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation. © Springer Science + Business Media, Inc. 2005 |
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Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction |
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Ji, Haisheng |
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| score |
7.403097 |