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Chapter 18: Problem 19

What sets the limits on the maximum and minimum masses of a main-sequence star?

Short Answer

Expert verified
The minimum and maximum masses of a main-sequence star are set by two limits: the minimum mass required for a star to sustain nuclear fusion at its core (around 0.08 solar masses), and the maximum mass before a star begins to blow apart due to overwhelming radiation pressure (around 100 solar masses).

Step by step solution

01

Understand the concept of a Main-Sequence Star

A main-sequence star is in a stable state where the forces of gravity pulling inward and the force of pressure pushing outward from the core are in balance. The energy that opposes gravity is produced by nuclear reactions in the core of the star. It is this balance that allows the star to maintain a stable size and temperature.
02

Identify the limits of a star's mass

The lower and upper limits of a main-sequence star's mass are determined by two factors: the minimum mass required for a star to generate energy through nuclear fusion of hydrogen atoms into helium (about 0.08 solar masses), and the maximum mass that a star can have without blowing apart due to its own radiation pressure (about 100 solar masses).
03

Explain the impact of mass on a star's life

The mass of a star determines its lifespan, energy output, and eventual fate. Lower mass stars will have longer lifetimes, less energy output but will eventually become white dwarfs. In contrast, massive stars have shorter lifetimes, a huge energy output, and will end their lives in a supernova explosion.

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Most popular questions from this chapter

Use the Starry Night Enthusiast \({ }^{\mathrm{TM}}\) program to examine the Milky Way Galaxy. Open the Favourites pane and click on Stars \(>\) Sun in Milky Way to display our Galaxy from a position \(0.150\) million light-years above the galactic plane. (You can remove the astronaut's feet from this view if desired by clicking on View \(>\) Feet.) You can zoom in or out on the Galaxy using the + and - buttons at the upper right end of the toolbar. You can move the Galaxy by holding down the mouse button while moving the mouse. You can also rotate the Galaxy by putting the mouse cursor over the image and holding down the Shift key while holding down the mouse button and moving the mouse. (a) You can identify H II regions by their characteristic magenta color. Describe where in the Galaxy you find these. Are most found in the inner part of the Galaxy or in its outer regions? (b) Where do you find dark lanes of dustin the inner part of the Galaxy or in its outer regions? Do you see any connection between the locations of dust and of H II regions? If there is a connection, what do you think causes it? If there is not a connection, why is this the case? You can examine the location of Galaxy in relation to neighboring galaxies by turning the Milky Way edge-on and by increasing the distance from the Earth using the up key below the Viewing Location on the toolbar.

Compare and contrast Barnard objects and Bok globules. How many Sun-sized stars could you make out of a Barnard object? Out of a Bok globule?

What are stationary absorption lines? In what sort of spectra are they seen? How do they give evidence for the existence of the interstellar medium?

Describe the energy source that causes a protostar to shine. How does this source differ from the energy source inside a main-sequence star?

Search the World Wide Web for recent discoveries about how brown dwarfs form. Do they tend to form in the same locations as "real" stars? Do they form in relatively small or relatively large numbers compared to "real" stars? What techniques are used to make these discoveries?
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