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Chapter 17: Problem 8

What is a planetary nebula? What happens to the core of a star after a planetary nebula occurs?

Short Answer

Expert verified
A planetary nebula is an expelled outer shell of a dying star; its core becomes a white dwarf.

Step by step solution

01

Understanding a Planetary Nebula

A planetary nebula is an astronomical phenomenon that occurs during the late stages of a star's life cycle. It happens when a star, typically similar in size to the Sun, exhausts its hydrogen fuel, leading to the expulsion of its outer layers into space. This creates a glowing shell of gas around the dying star core due to ionization by the remaining core's ultraviolet light.
02

Identifying the Core's Fate

After the outer layers are shed to form the planetary nebula, the core of the star remains. This core is incredibly dense and eventually cools over time. It becomes a white dwarf, which is a small, hot, and dense remnant of the star composed mainly of electron-degenerate matter.

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Key Concepts

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

White Dwarf
A white dwarf is the dense core left behind after a star has ejected its outer layers to create a planetary nebula. Despite its small size, which is comparable to Earth, a white dwarf can contain a mass similar to the Sun. This immense density makes it an intriguing object in the field of astronomy.
  • White dwarfs are incredibly hot when they first form.
  • They gradually cool over billions of years as they no longer perform nuclear fusion.
  • These remnants are primarily composed of electron-degenerate matter.
However, they remain visible because of their residual heat. Understanding white dwarfs helps astronomers comprehend the ultimate fate of stars like our Sun.
Star Life Cycle
A star undergoes a remarkable life cycle from its formation to its ultimate end. This cycle determines whether the star will become a white dwarf. Initially, a star forms from a collapsing cloud of gas and dust, where nuclear fusion ignites in its core, giving birth to a main-sequence star.
  • Main-sequence stars, like the Sun, spend most of their life fusing hydrogen into helium.
  • Once they exhaust the hydrogen, they expand into red giants.
  • The outer layers are eventually expelled to form a planetary nebula.
After these stages, the exposed core becomes a white dwarf, marking the final chapter in the life cycle of many stars. The star life cycle illustrates the transformative stages that stars undergo over billions of years.
Electron-Degenerate Matter
Within a white dwarf, the matter is no longer in the forms we typically encounter. Instead, it becomes electron-degenerate matter. This state occurs due to the immense gravitational pressure compressing the atoms so tightly that electrons are unwilling or unable to move freely, which means normal atomic interactions stop.
  • Electron-degenerate matter supports the white dwarf against further collapse.
  • This unique state allows the white dwarf to remain stable for a long period.
  • It is a fascinating example of quantum mechanical principles in astrophysics.
This exotic state of matter provides insight into how density and pressure can influence the composition and behavior of astronomical objects.

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Most popular questions from this chapter

When a star exhausts its core hydrogen fuel, the core contracts but the star as a whole expands. Why?

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Why is mass so important to a star's life? How and why do we divide stars into groups by mass?

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