Use Eq. (18.19) and Wien's law to make two log-log graphs: (1) the disk temperature, T(r), and (2) the peak wavelength [λmax(r)] of the blackbody spectrum, for the accretion disk around the black hole A0620−00 as a function of the radial position r. For this system, the mass of the black hole is 3.82M⊙, the mass of the secondary star 0.36M⊙, and the period of the orbit is 0.3226 day. Assume M˙=1014 kg s−1 (about 10−9M⊙ yr−1), and use the Schwarzschild radius, RS (Eq. 17.27), for the radius of the black hole. (On your graph, plot r/RS rather than r.) For a nonrotating black hole, the last stable orbit for a massive particle is at 3RS, so use this as the inner edge of the disk. Let the outer edge of the disk be determined by Kepler's third law along with Eqs. (18.25) and (18.26). On your log-log graph of λmax vs. r/RS, identify the regions of the disk that emit X-ray, ultraviolet, visible, and infrared radiation.