Development of an M6.4 Circular Solar Flare According to the Observations in the Нα Line
The development of the 3N/M6.4 flare on July 19, 2000, in the active region NOAA 9087 was studied based on the analysis of its images in the Н α line. Н α filtergrams obtained at the Meudon Observatory were used. The flare-active region NOAA 9087 had a complex multipolar magnetic field structure. Th...
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| creator | Chornogor, S. N. Kondrashova, N. N. |
| description | The development of the 3N/M6.4 flare on July 19, 2000, in the active region NOAA 9087 was studied based on the analysis of its images in the Н
α
line. Н
α
filtergrams obtained at the Meudon Observatory were used. The flare-active region NOAA 9087 had a complex multipolar magnetic field structure. The flare of 3N/M6.4 class began with the appearance of two bright kernels near a large spot. A few minutes later, flare kernels appeared in the central part of the active region, where a coronal source of hard X-ray radiation was identified. The flare lasted 2.5 h. Its energy was released sequentially in different places of the active region. The flare kernels were located along the polarity inversion line at the boundaries of the chromospheric cells. The flare ribbons had a circular shape. An assumption is made about the magnetic topology of the fan-spine type containing a null point. In this case, flare ribbons are the intersections of the fan quasi-separatrix layer with the lower atmosphere. The successive appearance of flare kernels may indicate a slipping magnetic reconnection in the flare. The Н
α
images in the main phase of the flare show reconnecting loops in the eastern part of the active region that are clearly visible in the ultraviolet wavelength range. |
| doi_str_mv | 10.3103/S0884591321020021 |
| format | Article |
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α
line. Н
α
filtergrams obtained at the Meudon Observatory were used. The flare-active region NOAA 9087 had a complex multipolar magnetic field structure. The flare of 3N/M6.4 class began with the appearance of two bright kernels near a large spot. A few minutes later, flare kernels appeared in the central part of the active region, where a coronal source of hard X-ray radiation was identified. The flare lasted 2.5 h. Its energy was released sequentially in different places of the active region. The flare kernels were located along the polarity inversion line at the boundaries of the chromospheric cells. The flare ribbons had a circular shape. An assumption is made about the magnetic topology of the fan-spine type containing a null point. In this case, flare ribbons are the intersections of the fan quasi-separatrix layer with the lower atmosphere. The successive appearance of flare kernels may indicate a slipping magnetic reconnection in the flare. The Н
α
images in the main phase of the flare show reconnecting loops in the eastern part of the active region that are clearly visible in the ultraviolet wavelength range.</description><identifier>ISSN: 0884-5913</identifier><identifier>EISSN: 1934-8401</identifier><identifier>DOI: 10.3103/S0884591321020021</identifier><language>eng</language><publisher>Moscow: Pleiades Publishing</publisher><subject>Astronomy ; Filtergrams ; Intersections ; Kernels ; Lower atmosphere ; Magnetic fields ; Magnetic reconnection ; Observations and Techniques ; Physics ; Physics and Astronomy ; Radiation ; Solar flares ; Solar Physics ; Spine ; Topology</subject><ispartof>Kinematics and physics of celestial bodies, 2021-03, Vol.37 (2), p.75-84</ispartof><rights>Allerton Press, Inc. 2021. ISSN 0884-5913, Kinematics and Physics of Celestial Bodies, 2021, Vol. 37, No. 2, pp. 75–84. © Allerton Press, Inc., 2021. Ukrainian Text © The Author(s), 2021, published in Kinematika i Fizika Nebesnykh Tel, 2021, Vol. 37, No. 2, pp. 41–56.</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><cites>FETCH-LOGICAL-c1831-cafcf16491d806bb9042e02524e6c32fa975a8ebdb77548803b8b79bc3945acc3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://link.springer.com/content/pdf/10.3103/S0884591321020021$$EPDF$$P50$$Gspringer$$H</linktopdf><linktohtml>$$Uhttps://link.springer.com/10.3103/S0884591321020021$$EHTML$$P50$$Gspringer$$H</linktohtml><link.rule.ids>314,778,782,27911,27912,41475,42544,51306</link.rule.ids></links><search><creatorcontrib>Chornogor, S. N.</creatorcontrib><creatorcontrib>Kondrashova, N. N.</creatorcontrib><title>Development of an M6.4 Circular Solar Flare According to the Observations in the Нα Line</title><title>Kinematics and physics of celestial bodies</title><addtitle>Kinemat. Phys. Celest. Bodies</addtitle><description>The development of the 3N/M6.4 flare on July 19, 2000, in the active region NOAA 9087 was studied based on the analysis of its images in the Н
α
line. Н
α
filtergrams obtained at the Meudon Observatory were used. The flare-active region NOAA 9087 had a complex multipolar magnetic field structure. The flare of 3N/M6.4 class began with the appearance of two bright kernels near a large spot. A few minutes later, flare kernels appeared in the central part of the active region, where a coronal source of hard X-ray radiation was identified. The flare lasted 2.5 h. Its energy was released sequentially in different places of the active region. The flare kernels were located along the polarity inversion line at the boundaries of the chromospheric cells. The flare ribbons had a circular shape. An assumption is made about the magnetic topology of the fan-spine type containing a null point. In this case, flare ribbons are the intersections of the fan quasi-separatrix layer with the lower atmosphere. The successive appearance of flare kernels may indicate a slipping magnetic reconnection in the flare. The Н
α
images in the main phase of the flare show reconnecting loops in the eastern part of the active region that are clearly visible in the ultraviolet wavelength range.</description><subject>Astronomy</subject><subject>Filtergrams</subject><subject>Intersections</subject><subject>Kernels</subject><subject>Lower atmosphere</subject><subject>Magnetic fields</subject><subject>Magnetic reconnection</subject><subject>Observations and Techniques</subject><subject>Physics</subject><subject>Physics and Astronomy</subject><subject>Radiation</subject><subject>Solar flares</subject><subject>Solar Physics</subject><subject>Spine</subject><subject>Topology</subject><issn>0884-5913</issn><issn>1934-8401</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2021</creationdate><recordtype>article</recordtype><recordid>eNp1UMtKAzEUDaJgrX6Au4DrqTevmWRZqlWh0kV142ZI0kyd0iY1mRb8GD_CHxE_yRkruBA358I9LzgInRMYMALscgZScqEIowQoACUHqEcU45nkQA5Rr6Ozjj9GJyktAUROFe-hpyu3c6uwWTvf4FBh7fF9PuB4VEe7XemIZ6HDcQsOD60NcV77BW4Cbp4dnprk4k43dfAJ1_779_n28Y4ntXen6KjSq-TOfm4fPY6vH0a32WR6czcaTjJLJCOZ1ZWtSM4VmUvIjVHAqQMqKHe5ZbTSqhBaOjM3RSG4lMCMNIUylikutLWsjy72uZsYXrYuNeUybKNvK8s2hRIKAopWRfYqG0NK0VXlJtZrHV9LAmU3YflnwtZD957Uav3Cxd_k_01fB7VyCA</recordid><startdate>20210301</startdate><enddate>20210301</enddate><creator>Chornogor, S. N.</creator><creator>Kondrashova, N. N.</creator><general>Pleiades Publishing</general><general>Springer Nature B.V</general><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>8FD</scope><scope>H8D</scope><scope>KL.</scope><scope>L7M</scope></search><sort><creationdate>20210301</creationdate><title>Development of an M6.4 Circular Solar Flare According to the Observations in the Нα Line</title><author>Chornogor, S. N. ; Kondrashova, N. N.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c1831-cafcf16491d806bb9042e02524e6c32fa975a8ebdb77548803b8b79bc3945acc3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2021</creationdate><topic>Astronomy</topic><topic>Filtergrams</topic><topic>Intersections</topic><topic>Kernels</topic><topic>Lower atmosphere</topic><topic>Magnetic fields</topic><topic>Magnetic reconnection</topic><topic>Observations and Techniques</topic><topic>Physics</topic><topic>Physics and Astronomy</topic><topic>Radiation</topic><topic>Solar flares</topic><topic>Solar Physics</topic><topic>Spine</topic><topic>Topology</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Chornogor, S. N.</creatorcontrib><creatorcontrib>Kondrashova, N. N.</creatorcontrib><collection>CrossRef</collection><collection>Meteorological & Geoastrophysical Abstracts</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Meteorological & Geoastrophysical Abstracts - Academic</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Kinematics and physics of celestial bodies</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Chornogor, S. N.</au><au>Kondrashova, N. N.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Development of an M6.4 Circular Solar Flare According to the Observations in the Нα Line</atitle><jtitle>Kinematics and physics of celestial bodies</jtitle><stitle>Kinemat. Phys. Celest. Bodies</stitle><date>2021-03-01</date><risdate>2021</risdate><volume>37</volume><issue>2</issue><spage>75</spage><epage>84</epage><pages>75-84</pages><issn>0884-5913</issn><eissn>1934-8401</eissn><abstract>The development of the 3N/M6.4 flare on July 19, 2000, in the active region NOAA 9087 was studied based on the analysis of its images in the Н
α
line. Н
α
filtergrams obtained at the Meudon Observatory were used. The flare-active region NOAA 9087 had a complex multipolar magnetic field structure. The flare of 3N/M6.4 class began with the appearance of two bright kernels near a large spot. A few minutes later, flare kernels appeared in the central part of the active region, where a coronal source of hard X-ray radiation was identified. The flare lasted 2.5 h. Its energy was released sequentially in different places of the active region. The flare kernels were located along the polarity inversion line at the boundaries of the chromospheric cells. The flare ribbons had a circular shape. An assumption is made about the magnetic topology of the fan-spine type containing a null point. In this case, flare ribbons are the intersections of the fan quasi-separatrix layer with the lower atmosphere. The successive appearance of flare kernels may indicate a slipping magnetic reconnection in the flare. The Н
α
images in the main phase of the flare show reconnecting loops in the eastern part of the active region that are clearly visible in the ultraviolet wavelength range.</abstract><cop>Moscow</cop><pub>Pleiades Publishing</pub><doi>10.3103/S0884591321020021</doi><tpages>10</tpages></addata></record> |
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| source | Springer Nature - Complete Springer Journals |
| subjects | Astronomy Filtergrams Intersections Kernels Lower atmosphere Magnetic fields Magnetic reconnection Observations and Techniques Physics Physics and Astronomy Radiation Solar flares Solar Physics Spine Topology |
| title | Development of an M6.4 Circular Solar Flare According to the Observations in the Нα Line |
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