Astronomers start their observations of this binary star system Upsilon Canum Ve

Question

Astronomers start their observations of this binary star system Upsilon Canum Venaticorum ( CVn) on Day 0 and observe the stars continually until the end of Day 4.5). In that time, they record the light levels of the stars and produce the light curve seen in Datasheet #1. What is the brightness (apparent magnitude) of the binary at the time of primary eclipse (secondary star eclipsing the primary), secondary eclipse (primary star eclipsing the secondary star), and out-of-eclipse (any point when the light of both stars can be seen from Earth)?

Explanation / Answer

From the light graph, we can conclude that the first dip belongs to a primary eclipse and the second dip belongs to the secondary eclipse because the primary star is bigger and brighter than the secondary star, so when the secondary star eclipse the primary star the dip in brightness is larger than the dip when secondary eclipse occurs.

So, from the graph the apparent magnitude

At the time of Primary eclipse is 7.15

At the time of Secondary eclipse is 6.25

At no eclipse is 5.35

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