a) Using the thermal radiation equation below and your knowledge of solar flux calculate theflux emitted from a star with a temperature of 6200 K to 2.d.p. Assume the star

is a perfectblack-body. The Stefan-Boltzmann thermal radiation equation is: P = AɛoTªWhere P= Power (W) ASurface area (m²) epsilon = Emissivity sigma =The Stefan-Boltzmann constant is 5.67 x 10-8 W · m2 . K-4= T = Temperature (K) (i) Explain, in this context, what is represented by the term 4ttr2? (ii) Explain, in this context, what is represented by the term a (iii) Redraw the diagram depicting the Earth's atmosphere as a single layer above theearth and add labels and direction arrows for the resultant fluxes (W/m2) under thoseconditions. (iv) Derive equations representing the temperature of the single atmospheric layer, and the temperature of the ground. State all the assumptions you have made.