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Chapter 17: Problem 15

Very young star clusters have main-sequence turnoffs a. that drop below the main sequence. b. at the top left of the main sequence. c. at the bottom right of the main sequence. d. in the middle of the main sequence.

Short Answer

Expert verified
b. at the top left of the main sequence.

Step by step solution

01

Understand the Main Sequence

The main sequence is a continuous and distinctive band of stars that appear on plots of stellar color versus brightness. Stars spend the majority of their lifecycle in this phase.
02

Understand Turnoff Points

Main-sequence turnoff points indicate where stars leave the main sequence to become red giants. This is associated with the age and evolution stage of a star cluster.
03

Very Young Star Clusters

Very young star clusters have not had much time to evolve. Consequently, their most massive stars, which are also the hottest and brightest, will be the first to leave the main sequence.
04

Determine Turnoff Location

Since the most massive, hottest, and brightest stars are situated at the top left of the main sequence, the turnoff point for very young star clusters will be at this location.
05

Conclusion

Based on the aforementioned points, the correct answer for the turnoff point location in very young star clusters is the top left of the main sequence.

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Key Concepts

These are the key concepts you need to understand to accurately answer the question.

Star Clusters
Star clusters are groups of stars that share a common origin and are gravitationally bound. They come in two main types: open clusters and globular clusters.
Open clusters are generally younger, containing hundreds to thousands of stars and are often found in the plane of the Milky Way. Globular clusters are older, more densely packed, and can contain up to hundreds of thousands of stars in a spherical shape.
Studying these clusters provides insight into stellar formation and evolution because all the stars in a cluster are approximately the same age and distance from Earth.
Stellar Evolution
Stellar evolution is the process by which stars change over time. The lifecycle of a star depends on its mass.
Stars are born in clouds of gas and dust called nebulae. When a nebula collapses under its gravity, it forms a protostar, which eventually ignites nuclear fusion in its core.
For most of their lives, stars are in the 'main sequence' phase, where they fuse hydrogen into helium. When hydrogen runs out, they leave the main sequence and evolve into red giants or supergiants, depending on their initial mass.
Main Sequence
The main sequence is the primary stage in a star's lifecycle. It is a continuous band on the Hertzsprung-Russell (H-R) diagram, which plots stars according to their brightness and temperature.
Stars on the main sequence are stable, fusing hydrogen into helium in their cores. They range from hot, massive, and bright stars at the top left of the H-R diagram to cooler, less massive, and dimmer stars at the bottom right.
The position of a star on the main sequence tells us about its mass and spectral type.
Red Giants
Red giants are a late stage in stellar evolution, occurring after a star exhausts the hydrogen in its core.
When a star leaves the main sequence, it expands and cools, increasing in size and turning red. This phase is called the red giant phase.
Red giants are significant because they shed their outer layers, enriching the surrounding space with heavier elements. This process plays a crucial role in the chemical evolution of galaxies, including forming planets and other stellar systems.
Understanding red giants helps astronomers learn about the future evolution of stars and the lifecycle of our universe.

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