| Name: | Pooja Devi |
| Affiliation: | Kumaun University Nainital |
| Conference ID : | ASI2024_908 |
| Title : | On the Relation between Prominence Eruptions and CMEs during Solar Cycle 24 |
| Authors : | Pooja Devi1, Nat Gopalswamy2, Seiji Yashiro2,3, Sachiko Akiyama2,3, Ramesh Chandra1,
Kostadinka Koleva2,3,4 |
| Authors Affiliation: | 1Department of Physics, DSB Campus, Kumaun University, Nainital 263 001, India
2NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
3The Catholic University of America, Washington, DC 20064, USA
4Space Research and Technology Institute, Bulgarian Academy of Sciences, Sofia, Bulgaria |
| Mode of Presentation: | Oral |
| Abstract Category : | Sun, Solar System, Exoplanets, and Astrobiology |
| Abstract : | We present the analysis of solar prominence eruptions (PEs) and related coronal mass ejections (CMEs) observed during the solar cycle 24 (May 2010-December 2019). We use data from the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) together with data from the Large Angle and Spectroscopic Coronagraph (LASCO) C2 coronagraph onboard Solar and Heliospheric Observatory (SOHO) spacecraft. The relation of PEs with CMEs is examined by setting a confidence level (CL) from 0 to 5 with 0 indicating no association and 5 indicating clear association. We found a total of 1225 (67% radial, 32% transverse, and 1% failed) PEs detected automatically from the SDO/AIA images. The average heights of all, radial, and transverse PEs are 1.31, 1.36, and 1.21 R⊙, respectively and their average speeds are ~ 38, 53, and 9 km s−1, respectively. Out of the 1225 PEs, 662 (54 %) are associated with CMEs; 69 % of these CMEs shows clear bright core structures for CL 1–5 and it becomes 78 % for CL 5. The average speed of PEs associated with CMEs, CME core, and CME leading edge are 62, 390, and 525 km s−1, respectively. Morphological and height-time analysis of PEs and CME cores reveals that the prominence material at greater height becomes the CME core. The temporal and spatial relationship between PEs and CMEs is solar cycle dependent. The temporal offset is large during solar maxima and small during minima. In the case of spatial relationship, it is found that during solar minima, the central position angle (CPA) of CMEs is closer to the equator than the PEs. This could be due to a strong polar field in the solar minimum. |
