ABSTRACT
The physics department at The University of North Texas is conducting a study of radio signals from our Sun. Radio Signals collected at a range of 1.4125X109 to 1.4175X109 were examined, along with signals outside this range, to search for a signature of the 21.11-cm hydrogen emission spectra. Monitoring of the sun spot activity of the sun is conducted with optical telescopes, internet searces and radio telescopes. The data, once collected was examined to search for any correlation between the sunspot cycle and the change in flux of the 21.11 cm emission spectra. Two signatures in the data were sought, one that was different from all the rest and another group showed a general trend. Sunspots are highly magnetized portions of the surface of the sun. With the increase in sunspot activity, there is also an increase in the magnetized portions of the surface of the sun and an increase in the 21.11-cm emission spectra is observed. Equations to predict the increase in flux corresponding to this spectra based on sunspot numbers are given in this work.