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/* Recurrent Novae */ Rewrote second sentence to be more clear.
==Recurrent Novae==
Recurrent novae are much like classical novae but are different as they are observed to have more then one outburst. Although most The terms classical novae are likely also the latter and recurrent novae may be interchangeable, as classical novae may have more than one outburst, given enough passage of time, making the categories interchangeable.
The amount of time between eruptions of a novae is determined by the original mass of the [[white dwarf]] itself, and thus the amount of accreted material required to trigger the outburst. [[Binary star|Binary stars]] with a white dwarf that has a mass of only 0.6 solar masses may take as long as 5 million years to accumulate enough material from its red giant companion before exploding as a nova. A white dwarf that is 1.3 solar masses on the other hand, may only take 30,000 years before accreting enough matter to have an outburst, having such eruptions every 30,000 years.
If a heavy white dwarf manages to accumulate enough additional mass to surpass its [[Chandrasekhar limit]] (1.4 solar masses) before the gas on the surface heats up sufficiently to cause a nova, the white dwarf itself will begin to collapse from the increased [[gravity]] and perish in a [[supernova#Type_1a|type-Ia supernova explosion]] instead.<ref>http://home.mindspring.com/~mikesimonsen/cvnet/id43.html</ref>
==Dwarf Novae==
