Question

What is the origin of the gas that can be seen as a planetary nebula around a hot, post-AGB star?

Short answer

The gas in a planetary nebula comes from the outer layers of a star ejected during the AGB phase.

Step-by-step solution

Understanding Planetary Nebula Formation

A planetary nebula is formed from the outer layers of a star that have been expelled. This process occurs in the late stages of a star's evolution when it transitions from the asymptotic giant branch (AGB) phase to a white dwarf.

Identifying the Source of the Gas

During the AGB phase, the star undergoes pulsations and strong stellar winds. These processes cause the star to lose mass and shed its outer layers, which is the gas that forms the surrounding nebula.

Condition of the Core during Nebula Formation

The core of the star, remaining after the outer layers are lost, becomes a hot, dense white dwarf. This leftover core heats the ejected gas and illuminates it to form the visible planetary nebula.

Key concepts

Asymptotic Giant Branch (AGB) Phase

The Asymptotic Giant Branch (AGB) phase is a stage in the life of a star that is up to several times more massive than our Sun. It's known as one of the last stages of stellar evolution for these stars. During this phase, the star has already exhausted the supply of hydrogen in its core.
The core contracts, resulting from gravitational forces, while nuclear reactions begin to burn helium in shells around the core. This process makes the star swell in size, sometimes reaching hundreds of times its original diameter. Stars in the AGB phase are characterized by:

• Strong stellar winds that cause the star to lose mass.
• Thermal pulsations from the different burning shells, leading to instability.
• A rich production of heavier elements that contribute to the composition of the interstellar medium after they are expelled.

The significance of the AGB phase is its role in enriching the universe with complex molecules and contributing to the mass loss that forms planetary nebulae.

Stellar Evolution

Stellar evolution is the process by which a star changes over time, extending from its formation to its death. It consists of several distinct stages, depending on the initial mass of the star. For low- to intermediate-mass stars, like our Sun, the evolutionary pathway includes:

• The Main Sequence Phase, where hydrogen fusion occurs in the core, providing energy and radiation pressure to combat gravity.
• Red Giant Phase, when the core runs out of hydrogen, causing the outer layers to expand and cool.
• The AGB Phase, which we covered earlier, characterized by pulsations and mass loss.

After the AGB phase, the star sheds its outer layers, forming a planetary nebula, and leaves behind a hot core. Understanding stellar evolution helps us to comprehend the lifecycle of stars and the recycling of material within galaxies. It also provides insight into the formation of different celestial phenomena, such as nebulae and white dwarf stars.

White Dwarf

A white dwarf is what remains after a star like our Sun expels its outer layers following the AGB phase. It represents the final stage of evolution for low and intermediate-mass stars. This remnant core is incredibly dense, composed mostly of electron-degenerate matter. Key characteristics of white dwarfs include:

• Extreme density, with a mass similar to the Sun but packed into a volume akin to Earth.
• High temperature initially, which gradually cools over billions of years.
• No fusion occurs within a white dwarf; its luminosity is due to residual thermal energy.

Despite their small size, white dwarfs play an important role in galaxies. They are the end state for most stars and contribute to our understanding of stellar life cycles. Over time, they can cool to become black dwarfs, although the universe is not old enough for any white dwarfs to have reached this stage yet.