Solar activities like coronal Mass Ejection (CMEs), solar flares and energetic particles control space weather. The most dominant form of solar activity is CMEs, and perhaps the primary source and driver of space weather. It is a striking manifestation of solar activity seen in solar corona (Gosling, 1993). CMEs constitutes large scale ejections of mass and magnetic flux from the lower corona into the interplanetary medium. Their masses are of the order of 1014 to 1017 g and speeds which can range from 100-3000 km/s (Webb and Howard, 2012). Although CMEs may have been caught a glimpse during the occasional total eclipse in the past thousands of years, and have been inferred in the early 20th century (Cliver, 1995) as an eruptive phenomena. They were discovered by the coronagraph on board the seventh Orbiting Solar Observatory (OSO -7) satellite on Dec. 14, 1971 (Tousey, 1973) which was 112 years after the first observation of solar flare. CMEs are generally known to consist of a three parts structure: frontal loop, a cavity and a core. A possible cause of CME generation is magnetic reconnection. It is thought to occur when two oppositely charged magnetic fields are brought together, they snap, and then the tremendous amount of energy stored in the oppositely directed magnetic field lines are released. This causes solar flare which drives CME (Reinard, 2008). A competing model of this magnetic reconnection model is the flux rope eruption mechanism (Schwenn, 2006)
Sunspots seem to also play main role in major solar activity. They appear as dark spot on the surface of the sun and have temperature as low as 4200k (in the central umbra) and 5700k (in the surrounding penumbra), compound to 6050k for the surrounding quiet photosphere, they are associated with bipolar magnetic loops that broke through the solar surface. Sunspots may divide or merge in a single or bipolar, may rotate; such motion may produce a large flare. Scientists believe that the number of spots on the sun, cycle over time reaching peak –the so called solar max, every 11 years or so. Sunspot cycle is understood to originate via a magnetohydrodynamic (MHD) dynamo mechanism involving complex interactions between plasma flows and magnetic fields in the solar convection zone (SC7) [Charbonneau, 2010]. Astronomers have been keeping track of the readily visible spots on the face of the sun for some 2500 years. Sunspots come in opposite polarities and begin in small groups approximately 30 degrees from the equator in both hemispheres. As the cycle progresses, the spots fades away and new ones appear closer and closer to the equator to eventually form something that can be illustrated in the so called butterfly diagrams.
Solar cycle certainly affects the upper atmosphere (stratosphere in particular). The ultraviolet light absorbed in this region fluctuate with the cycle of the solar activity. But how this solar cycle affects below the stratosphere is still a subject of debate.
Active regions on the sun, containing sunspot, and plagues are the primary source of CMEs. Closed magnetic field regions such as quiescent filament regions also cause CMEs; these secondary source regions can occur at all latitudes, but during the solar max, they occur predominantly at high latitudes, where sunspots are not found.
Several authors have reported that the time evolution of different solar activity parameters does not match together exactly. This has been attributed to the complex dynamics at different depths of the solar atmosphere (Kane, 2006). Since solar output affects our global environment [space weather, technology on earth, and the biosphere), there is urgent need to find solution to this complex dynamics. It has been postulated that this complex dynamics in the sun may be a chaotic process. Like every chaotic process, though difficult to find pattern in one or few studies, we are optimistic that many study of this nature will, in the near future, reveal an underlying regularity in this process.
Gopalswamy et al., (2003) reported on the mismatch between the peak occcurance of the halo CME rate and the SSN during the solar cycle 23, where the maximium halo CME rate occurred two years after the peak occurance of SSN. Rames & Rohimimi, 2008 noted that there are uncertainties in using sunspot numbers for predicting sunspot cycles. Munoz et al., 2010 statistically analyzed the dynamical parameters of solar ejections observed during solar cycle 23 (1996 to 2006), they compared their results with previous results and found extreme values which they attributed in some specific cases to higher sensibility of the instruments and to an overestimation of the values. Z.L. Du, (2011) investigated in detail the relationship and time delays between CME parameters and sunspot number (Rz) and found that they can be best describe by an integral response model. Nicewicz and Michalek (2016) statistically studied the properties of All CMEs (Jan 1996- Dec 2004) and found that CMEs do not only have different dynamic behavior but also different mass, width, velocity and acceleration. Onuchukwu, (2018) studied CME parameters and sunspot parameter for cycle 23 and found that the correlation between some of the Coronal Mass Ejection and sunspot parameters differs during the ascending and descending phases. Pant et al., (2021) investigated width distribution of slow and fast CMEs in solar cycle 23 and 24 and found that apart from their speeds, slow and fast CMEs are also distinctly different in terms of the distribution of their angular width in each case.
In this context, we are going to consider monthly time series solar activity and CME parameters for cycles 23 and 24. Monthly time series offers a more approximate result of variation than yearly time series. Because CMEs are ejected in active regions of the sun, it will be reasonable to compare their monthly average time series plots with the monthly time series plots of sunspot parameters. Also, we will consider distribution of CME parameters which will help us characterize them, and by plotting a normalized yearly time series of All CMEs and segregated CMEs used for this work, we would be able to establish trends between them.