The brightness, or luminosity, of each star relative to its companion can be determined from the light level along the bottom of the eclipse. From the spectroscopic data it has been determined that the cooler star is a K-type subgiant and the hotter star is a G-type mainsequence star. Since the primary eclipse is the eclipse of the hotter star by the cooler star, and since the cooler star is the larger, it can be seen from Figure 1 that all the light observed during totality must originate only from the cooler star. Therefore, the relative luminosity of the cooler star (Lc) in the SS Boo system can be directly determined by extending the eclipse bottom in Figure 2 toward the left until it intersects the yaxis. Read off the light level of this intersection to determine the value of Lc. Record your answer below.
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