Nova

A nova is a special event in space where a star suddenly becomes very bright and looks like a "new" star in the sky. This happens because of a star called a white dwarf that is very close to another star. The white dwarf pulls material from its companion star onto itself. When enough material builds up, it gets very hot and explodes, making the star look much brighter for a few weeks or months.

There are different kinds of novae. The most common type is called a classical nova. Another type, called a recurrent nova, can happen again after many years because the companion star keeps giving more material to the white dwarf. Sometimes, if too much material builds up, the white dwarf can explode completely, which is called a Type Ia supernova.

Novae usually appear along the path of the Milky Way in the night sky, but they can show up anywhere. They happen more often than bigger explosions called supernovae. Most novae need a telescope to see, but only a few become bright enough to see without one every dozen years or so. The last very bright nova was V1369 Centauri, which appeared in December 2013.

Etymology

In the 1500s, an astronomer named Tycho Brahe saw a bright new star in the sky. This star was in the constellation Cassiopeia. He wrote a book called De nova stella, which means "concerning the new star" in Latin. Because of this, people began to use the word nova to describe these bright new stars.

Even though the star Tycho saw was actually a supernova, the word nova stuck. Later, scientists learned that novae usually happen on objects called white dwarfs, which are what remains after very old stars have ended their lives.

Stellar evolution of novae

A nova happens when two stars orbit each other closely. One star becomes a small, dense remnant called a white dwarf. The other star spills material onto the white dwarf. This material builds up on the white dwarf's surface.

When enough material collects, a big reaction happens. The white dwarf bursts with bright light, looking like a new star. This light fades over weeks or months. Only a tiny bit of material is lost, and the white dwarf can burst again later. Sometimes, these bursts happen more than once, and the star is called a recurrent nova.

Occurrence rate and astrophysical significance

Astronomers think the Milky Way has about 25 to 75 novae each year, but we only see around 10 because space dust hides the others. As of 2019, 407 likely novae have been found in our galaxy. In the Andromeda Galaxy, about 25 bright novae are seen each year.

Studying novae helps us learn how they add elements like helium and lithium to space. They do not add as much material as bigger stellar explosions, but they still help make the material around us.

Some novae, like RS Ophiuchi, burst again every few decades, but most take much longer—thousands to hundreds of thousands of years—to repeat. The time between bursts depends more on the weight of the star than how fast it gathers material.

Subtypes

Novae are grouped by how quickly their brightness changes:

• NA: fast novae, which quickly grow bright and then dim to about 1⁄16 their peak brightness in under 100 days.
• NB: slow novae, taking 150 days or more to dim to that level.
• NC: very slow novae, which stay very bright for about ten years before slowly fading.
• NR/RN: recurrent novae, which have been seen to burst more than once within 80 years, and are usually fast.

Remnants

Some novae leave behind visible nebulosity. This is material thrown out during the explosion. Sometimes, this material looks like a cloudy area in the sky.

Novae as distance indicators

Novae help scientists measure distances in space. They shine very brightly and then slowly fade, acting like a special tool for measuring how far things are. Scientists know that novae usually have the same brightness 15 days after they first appear. This helps them figure out distances to nearby galaxies and groups of galaxies. These measurements are just as good as another way scientists use, which involves watching certain types of stars called Cepheid variable stars change in brightness.

Main article: standard candle
Main articles: Cepheid, variable stars

Recurrent novae

A recurrent nova is a star that shines very brightly many times. These stars usually become about 9 times brighter each time they erupt.

Scientists think that up to a quarter of all nova systems might erupt more than once, but only ten of these recurrent novae have been seen in our galaxy, the Milky Way. Some have also been observed in other galaxies, like the Andromeda Galaxy and the Large Magellanic Cloud. One of these, called M31N 2008-12a, can erupt as often as once every 12 months.

In April 2016, a website called Sky & Telescope reported that a star named T Coronae Borealis had been getting brighter since February 2015. This brightening happened before in 1938 and 1946. By June 2018, the star had dimmed a little but was still brighter than usual. In early 2023, it dimmed again. Some scientists thought it might shine very brightly again between March and September 2024, but as of May 19, 2026, this has not happened yet.

Extragalactic novae

Novae happen often in the Andromeda Galaxy (M31), including those that happen again and again. Each year, several dozen novae, which are very bright stars, are found in M31. The Central Bureau for Astronomical Telegrams (CBAT) keeps track of these novae in M31, M33, and M81.