Two stars can live close together.
Sometimes, one star grows very big. It can wrap around the other star. This makes a big cloud of gas. The stars move closer and closer. They might even become one star. Do you like looking at the stars?
Two stars can live close together.
Sometimes, one star grows very big. It can wrap around the other star. This makes a big cloud of gas.
The two stars move inside this cloud. The gas pulls on them. This makes the stars move closer. They might even crash and become one star. Or, the gas might fly away into space. This part of a star's life is very short. It is a big and fast change.
Sometimes, two stars live very close to each other. This is a binary star system.
One star might grow very large. It can fill its Roche lobe. A Roche lobe is the space around a star. When a star grows too big, it spills gas onto its neighbor. This can happen very fast. The gas builds up and wraps around both stars. This gas cloud is called a common envelope.
The two stars move inside this gas cloud. The gas creates drag forces. Drag is a force that slows things down. This drag makes the stars lose energy. Because they lose energy, they spiral inward. They move closer and closer to each other. This move is called a spiral-in.
This phase does not last long. It ends in one of two ways. First, the stars might merge. This means they crash to become one star. Second, the gas might be ejected. Ejection means the gas is thrown into space. This can leave two stars very close together. These close stars can later make gravitational waves.
A common envelope is a huge cloud of gas. It surrounds two stars in a binary star system.
This gas does not spin at the same rate as the stars. This stage is a very important part of how stars change. It can lead to many different kinds of space objects. Some systems end up as close double white dwarfs. Others become neutron stars or even black holes.
This special phase happens when one star grows very fast. The star fills its Roche lobe, which is its own space. It begins to spill gas onto its neighbor star. This process can happen too quickly for the second star to take it all. The extra gas builds up around both stars. Eventually, a common envelope forms and wraps around them both.
Inside the gas cloud, two objects continue to move. These are the core of the first star and its companion. The gas creates drag forces on these two objects. Drag is a force that slows things down. As the stars lose energy, they move into a closer orbit. This movement is called a spiral-in. The stars actually move faster as they get closer.
This stage is quite short compared to a star's life. It ends in one of two ways. The stars might merge to become a single star. Or, the gas might be ejected into space. If the gas is thrown away, the stars stay very close. Scientists have seen things like V1309 Scorpii. This event might show the ejection of a whole envelope.
These events are hard to see directly. They are often called luminous red novae. These events look brighter than a normal nova. They are fainter than a huge supernova. The gas cloud is relatively cool at about 5,000 K. This makes the light look red. These close star systems can even create gravitational waves.
In astronomy, a common envelope is a massive cloud of gas that surrounds a binary star system. A binary system consists of two stars orbiting one another. During a common-envelope phase, this shared gas does not rotate at the same rate as the stars inside it. This phase is a critical part of stellar evolution. It can fundamentally change the future of the stars involved. It can lead to the creation of very close binary systems or even single stars.
The process usually begins when one star in a binary system grows rapidly. As the star expands, it reaches a boundary called its Roche lobe. The Roche lobe is the specific region of space around a star where its gravity holds onto its material. When the star overfills this lobe, it begins mass transfer. This means gas spills from the expanding star onto its companion. This often creates a runaway process known as dynamically unstable mass transfer. The orbit shrinks, causing the star to overflow its Roche lobe even more. This cycle accelerates until the gas builds up around both stars, creating the common envelope.
Inside this thick gas cloud, the system contains two distinct objects. These are the core of the original donor star and its companion star. The donor's core does not expand along with the rest of the star's outer layers. As these two objects move through the gas, they experience drag forces. Drag is a force that resists motion. This drag causes the two objects to lose orbital energy. As they lose energy, they begin a spiral-in. This means they move into a much closer orbit. Interestingly, as the orbit shrinks, their orbital velocities actually increase.
The loss of orbital energy has a direct effect on the envelope itself. The energy lost by the orbiting objects is transferred to the gas. This process heats up and expands the common envelope. The entire common-envelope phase is quite short-lived compared to the total lifetimes of the stars. The phase eventually reaches an end through one of two primary outcomes. The first outcome is the ejection of the envelope into space. If the gas is expelled, the two stars remain as a binary system with a much smaller orbital separation. The second outcome is a merger. In a merger, the two objects become close enough to combine into a single star.
Scientists have identified several types of systems that likely resulted from this process. These include cataclysmic variables and X-ray binaries. We also see systems composed of close double white dwarfs or neutron stars. These systems all contain a compact remnant. A compact remnant is the dense core left behind after a star changes. These might be white dwarfs, neutron stars, or black holes. In these cases, the core was originally much larger than the current distance between the stars. The common-envelope phase explains how they reached such a close separation.
Observing these events is difficult because they happen so quickly. However, astronomers can infer their existence through specific signals. A common-envelope event should be brighter than a typical nova but fainter than a supernova. The photosphere, or the visible surface, of the envelope is relatively cool, around 5,000 K. This temperature causes the system to emit a red spectrum. Because the envelope is so large, it has a high luminosity. It can be as bright as a red supergiant. These events are sometimes called luminous red novae, or LRNe. They are a subset of intermediate-luminosity red transients.
There are several notable examples that help us understand this phenomenon. The event V1309 Scorpii is a possible example of the ejection of a whole envelope. Other observations, like M31 RV and V838 Monocerotis, are considered possible star mergers. We have also seen a planetary nebula that likely came from a common-envelope binary. These close-separation systems are also important for other areas of science. Short-period systems containing compact objects are sources of gravitational waves. They can also lead to Type Ia supernovae. Understanding the common envelope helps us understand the violent and complex life cycles of stars.
Where will your curiosity go next?
🖼️ Images & Media (2)
More to explore
✨ What else?
Related topics you might enjoy
🔬 Go deeper
More advanced topics to explore
What is Nepedia?
A free, ad-free encyclopedia for children. Every article is written at five reading levels, so the same page works for a five-year-old and a fifteen-year-old — use the level switcher above to see this one change. No account needed to read.