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The life of a Sun-like star

In about 5 billion years the Sun will swell into a red giant large enough to engulf Mercury and Venus.

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Step through the stages with the Stage slider or press Play. Change the mass menu to compare a red dwarf. Sizes in this view are not to scale; the readout gives typical sizes and times. At the white dwarf stage, the blue ball is Earth at the same scale.

Born in a cold cloud

Stars form in molecular clouds, vast regions of cold gas and dust. NASA describes them as holding from 1,000 to 10 million times the Sun's mass and spanning up to hundreds of light-years. Because the gas is cold, it clumps. Some clumps collide or gather more material, their gravity grows, and eventually they collapse. As a clump shrinks, it heats up and starts to spin faster, flattening the leftover gas into a disk. The hot, collapsing centre is a protostar. At this point its energy comes from the squeeze itself, not from fusion. The Sun formed this way about 4.6 billion years ago, and the disk around it became the planets.

When the core reaches millions of degrees, hydrogen fusion switches on and the outward push of energy halts the collapse. The star has joined the main sequence, the longest stage of its life. Mass sets the pace. NASA explains that more massive stars must burn their fuel faster to hold themselves up, so they shine brighter and die sooner, while low-mass stars burn longer, dimmer and cooler. The Sun's main-sequence life is about 10 billion years in total, and it is a little less than halfway through.

Running out of hydrogen

When the core runs out of hydrogen, fusion there stops and gravity wins for a while. The core shrinks and heats up, and hydrogen starts fusing in a shell around it. That extra energy makes the outer layers swell enormously and cool, and the star becomes a red giant, which NASA notes looks more orange than red. For the Sun this begins in about 5 billion years. NASA says the red giant Sun will become so large that it will engulf Mercury and Venus, and possibly Earth as well. Arcturus, about 25 Suns wide, shows what this stage looks like today.

Red giants become unstable and pulsate, puffing out and throwing off parts of their atmosphere. Eventually all the outer layers drift away as an expanding, glowing shell called a planetary nebula. The name dates from small telescopes in which these round shells looked a little like planets; they have nothing to do with planets. NASA's example is the Helix Nebula, 650 light-years away in Aquarius. What remains in the middle is the star's exposed core.

A white dwarf

That core is a white dwarf, usually about the size of Earth but hundreds of thousands of times more massive, as NASA puts it. It makes no new heat, so it slowly cools over billions of years, glowing from blue-white through to red. Sirius B is a nearby example: in the model, the Earth sitting next to the white dwarf at the same scale is slightly larger. Stars below about eight times the Sun's mass end this way, which covers the great majority of stars.

BackgroundRed dwarfs, the smallest true stars, do things differently. NASA explains that convection stirs the whole star, carrying fresh hydrogen down to the core, so a red dwarf can burn almost all its fuel without changing its structure. NASA says some red dwarfs with only about a third of the Sun's mass may last up to about 14 trillion years. The universe is only 13.8 billion years old, so not one red dwarf has run out yet. Because they live so long and are born in large numbers, NASA says red dwarfs make up about 75% of the stars in the Milky Way. Below them are brown dwarfs, 13 to 80 times Jupiter's mass, which never manage full hydrogen fusion and are not counted as stars.
cloudprotostarmain seq.red giantplan. nebulawhite dwarfblue main seq.supergiantsupernovaneutron starblack holeless than about 8 Sunsmore than about 8 Suns
The two main paths. Stars below about 8 solar masses end as white dwarfs; heavier stars explode as supernovae and leave neutron stars or black holes (next unit).
  • 4.6 billion years ago: The Sun forms from a collapsing cloud; the disk becomes the planets
  • Today: Main sequence, a little less than halfway through
  • In about 5 billion years: Core hydrogen runs out; the Sun swells into a red giant
  • After the giant stage: Outer layers drift off as a planetary nebula
  • Billions of years after that: An Earth-sized white dwarf slowly cools
  1. Where do stars form?
    • In cold molecular clouds of gas and dust
    • Inside planets
    • In the hot corona of the Sun
    • In black holes
  2. Where does a protostar's energy mainly come from?
    • Heat released by its own collapse
    • Hydrogen fusion
    • Burning carbon like coal
    • Sunlight from nearby stars
  3. Which star lives longer?
    • A low-mass red dwarf
    • A massive blue star
    • They live equally long
    • Whichever is closer to Earth
  4. The Sun is 4.6 billion years old with about 5 billion years left on the main sequence. Total main-sequence life in billions of years? (one decimal)
  5. What happens when the Sun's core runs out of hydrogen?
    • The core shrinks and heats; the outer layers swell into a red giant
    • The Sun explodes as a supernova at once
    • The Sun turns into a black hole
    • Nothing changes
  6. A planetary nebula is ...
    • the outer layers of a dying star drifting away
    • a cloud where planets are forming
    • a planet with a glowing atmosphere
    • a small galaxy
  7. About how big is a typical white dwarf?
    • About the size of Earth
    • About the size of the Sun
    • About the size of Jupiter's orbit
    • About the size of a city
  8. Why has no red dwarf run out of fuel yet?
    • Their lifetimes are far longer than the 13.8-billion-year age of the universe
    • They are refuelled by comets
    • They do not use fusion
    • They all exploded long ago
  9. What percentage of the Milky Way's stars are red dwarfs, according to NASA?
  10. Put the Sun's stages in order.
Key points
  • Stars form when clumps in cold molecular clouds collapse.
  • Fusion starts the main sequence, the longest stage; mass sets the lifetime.
  • The Sun: about 10 billion years on the main sequence, now a little under halfway.
  • Then red giant, planetary nebula, and an Earth-sized white dwarf.
  • Red dwarfs (about 75% of Milky Way stars) last trillions of years.
Sources for this course (14)
  • NASA Sun Fact Sheet (nssdc.gsfc.nasa.gov/planetary/factsheet/sunfact.html)
  • NASA Sun facts (science.nasa.gov/sun/facts)
  • NASA Stars (science.nasa.gov/universe/stars)
  • NASA Star types (science.nasa.gov/universe/stars/types)
  • NASA What is Betelgeuse (science.nasa.gov/universe/what-is-betelgeuse-inside-the-strange-volatile-star)
  • NASA Hubble Betelgeuse dimming (science.nasa.gov/missions/hubble/hubble-finds-that-betelgeuses-mysterious-dimming-is-due-to-a-traumatic-outburst)
  • NASA Marshall Watch the Skies Betelgeuse (nasa.gov/blogs/watch-the-skies/2024/09/06)
  • ESA/Hubble Sirius B (esahubble.org/news/heic0516)
  • NASA Hubble Sirius asset (science.nasa.gov/asset/hubble/the-dog-star-sirius-and-its-tiny-companion)
  • NASA SVS Alpha Centauri (svs.gsfc.nasa.gov/20377)
  • ESA Gaia HR diagram (sci.esa.int/web/gaia/-/60198-gaia-hertzsprung-russell-diagram)
  • NASA Imagine the Universe Life Cycles of Stars (imagine.gsfc.nasa.gov/educators/lifecycles/LC_main3.html)
  • NASA Chandra HR diagram (chandra.harvard.edu/edu/formal/variable_stars/bg_info.html)
  • NASA Space Math spectral classes (spacemath.gsfc.nasa.gov stars 5Page43).

Checked: 2026-10-17