Novae and Type I Supernovae

Sometimes, when a white dwarf forms, it is in a binary (or multiple) star system. If the companion star is close enough, the white dwarf call pull some of the material off the companion, and accrete it onto the surface of the white dwarf.


When the stellar material hits the hot surface of the white dwarf, the material can fuse quickly and create what is called a nova. Novae are not as energetic as supernovae, but will increase the luminosity greatly. However, the material accreted is rapidly used up and the nova dies down. Nova can occur many times and do have a predictable period that can be measured.


However, if the material on the surface of the white dwarf accretes too fast, the material can increase the mass of the white dwarf to over the Chandrasekhar limit. When this happens, instead of a nova explosion, the white dwarf undergoes a catastrophic collapse. What occurs is a Type I Supernova.


Since the white dwarf mass becomes larger than 1.4 solar masses, the electron degeneracy of the white dwarf cannot overcome the gravity the white dwarf experiences. The white dwarf catastrophically collapses, allowing all the material in the white dwarf to fuse rapidly. The outward explosion from this sudden release of energy completely destroys the white dwarf and companion star. The way astronomers differentiate between Type I Supernovae and Type II Supernovae is the lack of hydrogen lines in Type I. Because the white dwarf has no remaining hydrogen and the hydrogen from the companion star is completely used up in the fusion process, we know that Type I Supernovae can only be created by the sudden collapse of a white dwarf that accretes material from a companion star.

From Wikipedia, OOCalc chart

Looking at the above image, another difference between Type I and Type II supernova is that Type I are typically much brighter in the beginning but fade much quicker.

White Dwarfs

White dwarfs are the stellar remnants of low- to medium-mass main sequence stars.




Typically, once these stars can no longer fuse hydrogen in their cores, gravity will take over, compress the core, and increasing its temperature. This, in turn, allows the fusion of helium into carbon via the triple-alpha process. As the heat from the core increases, it pushes the outer layers of the star out, making the star a Class III (giant) star. When the helium in the core stops fusing, the outer layers collapse again and recompress the core. The temperature of the core will not get hot enough to fuse the carbon (and possibly nitrogen and oxygen) into anything heavier. Instead, something else will occur.




The outer layers will be pushed out and off the star but the rebound of the core. What is left are the naked core (the white dwarf) and the outer layers of the star which becomes a planetary nebula. The planetary nebula is named such because when they were first discovered, they were thought to be the beginning of a solar system. After initial observations, the first planetary nebulae were discovered to have a white dwarf at the center.

Helix Nebula. Note the white dot at the center. This is the white dwarf

Image Credit:

NASA, NOAO, ESA, the Hubble Helix Nebula Team, M. Meixner (STScI), and T.A. Rector (NRAO)

White dwarfs, themselves, are basically dying stars. Fusion no longer takes place on or in white dwarfs. All that happens is that the white dwarf is slowly cooling down. Since the white dwarf is the core of a star, the white dwarf is initially very hot, which is why they are on the left side of the HR Diagram. But they are also very small, so extremely dim. White dwarfs are mostly carbon, since that was the last material that was created in the core. Also, white dwarfs are very dense. They have a radius similar to Earth's radius, but with a mass comparable to the Sun. A teaspoon of white dwarf material weighs several tons.


What makes the white dwarf stable is something called electron degeneracy. Electron degeneracy is the electromagnetic force from electrons in a confined space counteracts the gravity wanting to squash the white dwarf. However, there is a limit to the mass that will be stable with electron degeneracy. This limit is called the Chandrasekhar limit and is around 1.4 solar masses. Any higher, and the white dwarf will collapse farther and lead to a Type I supernova (later topic). Any main sequence star with an initial mass of 10 solar masses or lower will end up as a white dwarf.

.Sirius A and B (with Sun for comparison). Sirius B is the closest known white dwarf to the Sun

Image Credit:

Astro Bob