Coronal mass ejection

The most energetic occurrences in the solar environment are called coronal mass ejections (CMEs). The Seventh Orbiting Solar Observatory (OSO-7) was used to detect CMEs for the first time in coronagraph photos in 1971 (Tousey 1973). To examine the faint corona structures outside the occulting disc's periphery in the photospheric light dispersed by these structures, most coronagraphs use an occulting disc to intentionally eclipse the bright photosphere. Today's astrophysics is studying the Sun's huge and perpetually active environment, which is a result of the Sun's magnetic field's ongoing alterations. The Sun undergoes surface changes over the course of its 11-year cycle, and its magnetic flux has a significant impact on the entire environment. The 11-year term was originally used to define the sunspot number change (Schwabe et al., 1844). Solar cycle 25, which started in December 2019 and is the one we are presently in, is more potent than solar cycle 24. When coronal mass ejections (CMEs) leave the solar atmosphere and enter the heliosphere, they do so at speeds that can range from 100 to 3,000 km/s Yashiro et al. (2004). In the coronagraph field of view (FOV), they appear as white-light features that are brilliant and move outward (Hundhausen et al., 1984). Tousey et al., (1973) was the first to notice CMEs in coronagraph images, despite the fact that the earliest observations of CMEs were made in the 1970s (Hansen et al., 1971) (see a recent study of the history of CMEs by Gopalswamy et al., (2016)).CMEs are regularly tracked by the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI) on the Solar Terrestrial Relation Observatory(STEREO) (Howard et al., 2008). The sun's closed magnetic areas, active regions, filament regions, active region complexes, and Tran’s equatorial linking regions are the sources of CMEs, which are large-scale magnetized plasma structures. CMEs have posed a serious threat to the upper atmosphere's dynamic and unpredictable circumstances. According to studies conducted over the past fifty years, CMEs constitute the heliosphere's most energetic event (Gopalswamy et al., 2006; Richardson et al., 2000).Although the resolution of the SECCHI sensor prevents us from seeing it, it's likely that certain narrow CMEs do have observable structure. The narrow CMEs appear to be mass flows in vertical flux tubes, according to another observation. They looked into the narrow CME's characteristics and discovered that they occur more frequently as the sun approaches its maximum (Yashiro et al., 2003). They demonstrated that the average speed of intermediate CMEs increases from 146 km/s during the solar ascending phase (2009–2010) to 2268 km/s at the solar maximum phase (2012– 2013). They also considered the angular width (20º <W<200º) for intermediate CMEs (Mittal et al., 2009). (Yashiro et al., 2008) analysed the statistical characteristics of 24th cycle CMEs by automatic and manual approach, in which they omitted the CMEs with angular width 30o since such CMEs are very subjective. They discovered certain differences between intermediate and normal CMEs. Our main goal in this work is to evaluate how the features of these three groups vary from one solar cycle to the next while examining the speed, angular width, and linear speed of intermediate and wide CMEs throughout solar cycles 24 (2008-2012) and 25 (2019-2022).We analysed the angular width and linear speed of all kinds of CMEs, including intermediate (20º<W<200º), wide (W≥ 200º), and linear speed 500 km/s, during the ascending phase of solar cycles 24 and 25.Solar cycle 24 has intermediate CME 434 which is 4.5 times more than solar cycle 25. On the other hand, there was no noticeable difference in the number of large CMEs during solar cycles 24 and 25 (405 and 406, respectively). The striking finding is that the angular distributions for the ascending phase of solar cycles are quite similar. The maximum speed observed during ascending phase of solar cycle 24 is 2658 km/s (wide) and the maximum speed in ascending phase of solar cycle 25 is 2669 km/s (wide). The maximum number of wide Coronal Mass Ejections are occurred in the year of 2022.It was noticed that the maximum speed of solar cycle 24 is higher than the solar cycle 25.