mperature of about 5,500 K which contrasts to the photospheric temperature of 6,000 K. The difference intemperatures makes the sunspots appear dark against the brightness of thephotosphere (Nicolson 123). A sunspot’s average size is comparable with the Earth. They form inregions of concentrated magnetic fields. These fields hamper the flow of energyto the affected area. The magnetic fields on the Sun are detected by theZeeman effect, which shows a single spectral line that splits if a magnetic field ispresent (Nicolson 124). In each sunspot pair in the northern hemisphere the firstspot has a north magnetic polarity and the second has a south magnetic polarity{figure 1}, while in the southern hemisphere it is the opposite pattern. In sunspotgroups the polarity of the sunspots gets increasingly complex (Nicolson 124). The sunspots follow a cycle of eleven years. The number of sunspotsvaries monthly from zero to the hundreds. During the eleven year cycle there areperiods called solar maximum and solar minimum where the number of sunspotsreaches its peak or low. At the time of solar max the Sun’s magnetic polesreverse. The north magnetic pole switches to extend through the southernhemisphere and the south magnetic pole extends through the northernhemisphere. In fact the Sun reached its solar max in February of this year(Philips 1).According to astrophysicist, K. V. K. Nehru the magnetic poles reversebecause of a theory of high range temperature matter. His theory states thatone way high temperature matter acts in is thredules, which is “[m]atter in theultra high temperature range manifests as slender, unidirectional, expandingthreads that keep forming and dissolving” (1Nehru 8). Nehru states thatco-magnetic lines follow the thredules as they expand. North and souththredules form two “sheaves” one north polarized and one south polarized, butwhere the sheaves interact opposite polarities a...
