A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734
We present a detailed analysis of a partial eruption of a sigmoid filament lying along the polarity inversion line (PIL) of the small active region (AR) NOAA 12734 (with an area of 1.44 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline">...
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| Format: | Article |
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MDPI AG
2024-01-01
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| Series: | Universe |
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| Online Access: | https://www.mdpi.com/2218-1997/10/1/42 |
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| author | Jihong Liu Yin Zhang Yuhong Zheng Yu Liu Jie Chen |
| author_facet | Jihong Liu Yin Zhang Yuhong Zheng Yu Liu Jie Chen |
| author_sort | Jihong Liu |
| collection | DOAJ |
| description | We present a detailed analysis of a partial eruption of a sigmoid filament lying along the polarity inversion line (PIL) of the small active region (AR) NOAA 12734 (with an area of 1.44 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>×</mo><mspace width="3.33333pt"></mspace><msup><mn>10</mn><mn>3</mn></msup></mrow></semantics></math></inline-formula> square megameters). The active filament was rooted in a dipole sunspot of the AR. The eruption was associated with a C1.3 flare and subsequent large-scale coronal disturbances. During its solar disk passage before the flare, the AR had the following characteristics: (1) Most of the time, the magnetic field lines in the AR showed a sigmoidal structure (‘L1’) in the low corona and arc-shaped loops (i.e., ‘L2’) in the upper atmosphere. (2) An ‘X’-shaped structure was formed between the original ‘S’-shaped magnetic loop (‘L1’) and the newly rising one (‘L3’) between the main positive and negative magnetic polarities of the sunspots, and the intersection point of flux ropes ‘L1’ and ‘L3’ corresponds well with the area where the initial extreme-ultraviolet (EUV) 1600 Å brightening of the flare occurred. (3) The AR disobeyed the hemispherical helicity rule and had magnetic twist and writhe of the same signs, i.e., its magnetic helicity/current helicity were positive in the northern hemisphere. (4) Sustained magnetic emergence and cancellation occurred before the flare. Therefore, the magnetic reconnection of highly twisted helical flux ropes under the confinement of the overlying magnetic fields is probably responsible for the partial eruption of the filament. |
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| id | doaj.art-50fdb98e94b6431c8faf6330843647ca |
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| issn | 2218-1997 |
| language | English |
| last_indexed | 2024-03-08T10:33:20Z |
| publishDate | 2024-01-01 |
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| series | Universe |
| spelling | doaj.art-50fdb98e94b6431c8faf6330843647ca2024-01-26T18:43:06ZengMDPI AGUniverse2218-19972024-01-011014210.3390/universe10010042A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734Jihong Liu0Yin Zhang1Yuhong Zheng2Yu Liu3Jie Chen4School of Science, Shijiazhuang University, Shijiazhuang 050035, ChinaNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, ChinaShijiazhuang Post and Telecommunications Technical College, Shijiazhuang 050011, ChinaSchool of Physical Science and Technology, Southwest Jiaotong University, Chengdu 610031, ChinaNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, ChinaWe present a detailed analysis of a partial eruption of a sigmoid filament lying along the polarity inversion line (PIL) of the small active region (AR) NOAA 12734 (with an area of 1.44 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>×</mo><mspace width="3.33333pt"></mspace><msup><mn>10</mn><mn>3</mn></msup></mrow></semantics></math></inline-formula> square megameters). The active filament was rooted in a dipole sunspot of the AR. The eruption was associated with a C1.3 flare and subsequent large-scale coronal disturbances. During its solar disk passage before the flare, the AR had the following characteristics: (1) Most of the time, the magnetic field lines in the AR showed a sigmoidal structure (‘L1’) in the low corona and arc-shaped loops (i.e., ‘L2’) in the upper atmosphere. (2) An ‘X’-shaped structure was formed between the original ‘S’-shaped magnetic loop (‘L1’) and the newly rising one (‘L3’) between the main positive and negative magnetic polarities of the sunspots, and the intersection point of flux ropes ‘L1’ and ‘L3’ corresponds well with the area where the initial extreme-ultraviolet (EUV) 1600 Å brightening of the flare occurred. (3) The AR disobeyed the hemispherical helicity rule and had magnetic twist and writhe of the same signs, i.e., its magnetic helicity/current helicity were positive in the northern hemisphere. (4) Sustained magnetic emergence and cancellation occurred before the flare. Therefore, the magnetic reconnection of highly twisted helical flux ropes under the confinement of the overlying magnetic fields is probably responsible for the partial eruption of the filament.https://www.mdpi.com/2218-1997/10/1/42flaresfilaments/prominencesmagnetic fieldsreconnection |
| spellingShingle | Jihong Liu Yin Zhang Yuhong Zheng Yu Liu Jie Chen A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734 Universe flares filaments/prominences magnetic fields reconnection |
| title | A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734 |
| title_full | A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734 |
| title_fullStr | A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734 |
| title_full_unstemmed | A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734 |
| title_short | A Partial Eruption of a Sigmoid Filament in the Small Dipole Active Region 12734 |
| title_sort | partial eruption of a sigmoid filament in the small dipole active region 12734 |
| topic | flares filaments/prominences magnetic fields reconnection |
| url | https://www.mdpi.com/2218-1997/10/1/42 |
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