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Chapter 15: Problem 17

The Hayashi track is a nearly vertical evolutionary track on the H-R diagram. What does the vertical nature of this track tell you about a protostar as it moves along it? a. The star remains the same brightness. b. The star remains the same luminosity. c. The star remains the same color. d. The star remains the same size.

Short Answer

Expert verified
b. The star remains the same luminosity.

Step by step solution

01

Understanding the H-R Diagram

The Hertzsprung-Russell (H-R) diagram plots stars based on their luminosity and temperature (or color). The vertical axis usually represents luminosity, and the horizontal axis represents temperature or color.
02

Interpreting the Hayashi Track

The Hayashi track is a nearly vertical line on the H-R diagram that protostars follow as they evolve. Since the track is vertical, the horizontal coordinate, representing temperature or color, changes, while the vertical coordinate, representing luminosity, remains constant.
03

Conclusion from the Hayashi Track

Given that the Hayashi track is nearly vertical, it indicates that the luminosity of the protostar remains the same as it evolves along this track. Therefore, the correct interpretation is that the star remains the same luminosity.
04

Choosing the Correct Answer

Among the given options, the statement that 'the star remains the same luminosity' (option b) is correct.

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Key Concepts

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

H-R Diagram
The Hertzsprung-Russell (H-R) diagram is a stellar chart that plots stars based on two main properties: luminosity and temperature. On the vertical axis, you鈥檒l find luminosity, which measures how much energy a star emits. The horizontal axis shows temperature, with hot stars (blue) on the left and cooler stars (red) on the right. Also, temperature correlates with the star's color. This diagram helps astronomers understand different stages of stellar evolution and group stars with similar features.
Protostar Evolution
A protostar is an early stage in the formation of a star. It forms from a collapsing cloud of gas and dust in space. As the protostar continues to contract under gravity, it gets hotter and denser. This phase is depicted on the H-R diagram by the Hayashi track. The movement along this track is crucial to understand. As the protostar evolves, it changes in temperature while maintaining its luminosity.
Stellar Luminosity
Stellar luminosity is the amount of energy a star emits per second. On the H-R diagram, this is represented on the vertical axis. Luminosity is essential because it tells us about the star's energy output. For a protostar on the Hayashi track, the vertical nature of the track means that the star鈥檚 luminosity stays constant despite other changes happening within the star. This insight helps astronomers predict how much energy the star emits during this phase.
Stellar Temperature
Stellar temperature is a measure of how hot the surface of a star is. Temperature correlates with the color of the star, where hotter stars appear blue and cooler stars appear red. On the H-R diagram, temperature is shown on the horizontal axis. When a protostar moves along the Hayashi track, its temperature changes. This change in temperature reflects the different stages of the protostar鈥檚 evolution and indicates how the star is cooling and contracting over time.
Stellar Formation
Stellar formation is the process by which a star is born from a molecular cloud of dust and gas. This process includes several stages, starting from the initial collapse of the cloud to form a protostar, and leading to the main sequence phase where the star begins nuclear fusion. During the early stages, the protostar follows the Hayashi track on the H-R diagram, which shows how its temperature changes while its luminosity remains constant. Understanding these stages is vital for learning how stars develop and evolve over time.

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Most popular questions from this chapter

Astronomers understand the process of star formation because a. they have observed star formation as it happens for a small number of stars. b. they have observed star formation as it happens for a large number of stars. c. they have observed many different stars at each step of the process. d. theoretical models predict that this must be the way stars form.

Astronomers know that there are dusty accretion disks around protostars because a. there is often a dark band across the protostar. b. there is often a bright band across the protostar. c. theory says accretion disks should be there. d. there are planets in the Solar System.

Go to the website for Stardust (http://stardustathome.ssl berkeley.edu), a Citizen Science project that asks Internet users to use a virtual microscope to analyze digital scans of particles collected by the Stardust mission in \(2006 .\) The goal is to identify tiny interstellar dust grains. Follow the four steps under "Get Started" (you need to create a log-in account) and help search for stardust. Click on "News." What has been learned from this project? Remember to save the images for your homework, if required.

Molecular hydrogen is very difficult to detect from the ground, but astronomers can easily detect carbon monoxide (CO) by observing its 2.6 -cm microwave emission. Describe how observations of CO might help astronomers infer the amounts and distribution of molecular hydrogen within giant molecular clouds.

If a typical hydrogen atom in a collapsing molecular-cloud core starts at a distance of \(1.5 \times 10^{12} \mathrm{km}(10,000 \mathrm{AU})\) from the core's center and falls inward at an average velocity of \(1.5 \mathrm{km} / \mathrm{s},\) how many years does it take to reach the newly forming protostar? Assume that a year is \(3 \times 10^{7}\) seconds.
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