Solar activity refers to any natural phenomenon occurring on the sun such as sunspots, solar flare and coronal mass ejection etc. Such phenomena have their roots deep inside the sun, where the dynamo mechanism operates and fluid motions occur in a turbulent way. It is mainly driven by the variability of the sun’s magnetic field. The present paper studies the relation between various solar features during January 2009 to December 2011. A good correlation between various parameters indicates similar origin.
The solar atmosphere continues to be one of the richest and most dynamic environments studied in modern astrophysics. Spanning many orders of magnitude in density and temperature, while linked to the complex system of magnetic field the sun displays a myriad of interesting phenomenon from sunspots in the photosphere to coronal mass ejections—the most energetic events in the solar system. Like earth, the sun has seasons. More precisely, it has a cycle that lasts about 11 years. The number of sunspots rises and falls and rises again in about 11 years. This is due to the variability of solar magnetic field. The variability of the magnetic field has a strong influence on the dynamics of the outer layer of the sun and is registered by several solar parameters such as the sunspot number, the rate at which flux and coronal mass ejections occur, the flux of solar X-rays and radio waves.
The wealth of solar coronal phenomena called as solar activity should be viewed beyond their individual occurrences [
They suggested that this relation is independent of the phase of the solar activity cycle and predicted a rate of 3.2 per day for solar maximum phase.
Webb & Howard [
Researchers have studied the solar cycle that ended in December 2008 which is known as solar cycle 23. This cycle was longer than normal. The present solar cycle 24 started in December 2008 and is expected to have a shorter time period. In this paper we have studied the relation between various solar features during January 2009 to December 2011 for this cycle.
Data were obtained from the SOHO-LASCO CME catalogue http://cdaw.nasa.gov/cme_lis/index.html,from the NOAA websites ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/SUNSPOT_NUMBERS/INTERNATIONAL; ftp://ftp.ngdc.noaa.gov/STP/SOLAR_DATA/Flux/penticon_observed,and ftp://ftp.ngdc.noaa.gov/STP/SOLAR_ DATA/Satellite_enviornment/XRay_BGND/GOESBGND.o6 for coronal mass ejection frequency, for sunspot number,for 2800 MHz solar radio emission,and for solar X-ray background, in that order.