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Optical astronomers discovered CVs based on their outbursts in the middle of the 19th century. CVs are classified into subclasses according to the properties of the outbursts: classical novae and dwarf novae. Classical novae are seen to erupt once, and the amplitude of the outburst is the largest among CVs. Classical nova outbursts are caused by sudden nuclear fusion of hydrogen-rich material on the surface of the white dwarf. Because white dwarfs are the cinders of stars like the Sun, hydrogen fusion is possible only when fresh fuel is accreted onto its surface.
Dwarf novae outbursts result from temporary increases in the rate of accretion onto the white dwarf, caused by the additional material accreted onto the surface. This material must go through a violent transition region called the "boundary layer", which lies just above the surface of the white dwarf. Dwarf novae outbursts are smaller in amplitude and higher in frequency than classical novae. The variable star U Geminorum, or "U Gem," is the prototype of dwarf novae. The brightness in the visible light of U Gem increases by a hundredfold every 120 days or so, and returns to the original level after a week or two.
Optical astronomers have also recognized "recurrent novae," which are eruptive behaviors that fall between the definitions of classical and dwarf novae, and "nova-like systems," which are stars that have similar spectra to other types of CVs in the visual light, but have not been seen to erupt.
In some cases, nuclear fusion, rather than accretion, can become the dominant energy source in a CV. The case of the classical nova outburst has been mentioned above. In addition, X-ray astronomers have discovered a class of objects called the "super-soft sources" (or SSS): the name derived from the X-ray spectrum of these systems, which is dominated by soft (lower energy) X-ray photons, typically below 0.5 keV. Detailed studies of the spectra of these SSS have revealed that they have the characteristic of X-rays from the hot (T 200,000 - 800,000K), high gravity (g 1,000,000 m/s/s) surface of a star. Such high gravity implies a white dwarf more massive than our Sun, which has its own implications.
Though some matter is ejected during a nova, some may also be retained, so the accretion/nova cycle can still allow for the dwarf's mass to increase. This mass gain could eventually result in the dwarf reaching the Chandrasekhar limit of 1.4 solar masses. As it approaches that limit, pressure builds and the internal temperature rises enough for carbon fusion to begin. The majority of white dwarfs are composed mostly of carbon, and when this fusion occurs, all the carbon undergoes fusion instantly. The result is a white dwarf supernova.
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