History of Nova

	Revision 8 . . (edit) October 16, 2001 12:41 pm by Bryan Derksen [removed extraneous "either"]
	Revision 7 . . (edit) October 16, 2001 10:02 am by Paul Drye [Type Ia, not 1a (roman, not arabic numeral)]
	Revision 5 . . October 16, 2001 8:30 am by Josh Grosse [Correction, but somebody check this]

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Difference (from prior major revision) (minor diff, author diff)

Changed: 7c7

A white dwarf can potentially generate multiple novae over time as additional hydrogen continues to accrete onto its surface from its companion star. Eventually, however, the white dwarf will either undergo a nova so powerful that it is completely destroyed in the process, or the companion star will run out of hydrogen for the white dwarf to pull away. This is one type of supernova, though others can occur through entirely different processes.

A white dwarf can potentially generate multiple novae over time as additional hydrogen continues to accrete onto its surface from its companion star. Eventually, however, either the companion star will either run out of material, or the white dwarf will undergo a nova so powerful that it is completely destroyed in the process. This is somewhat similar to a type Ia supernova. Supernovae in general, however, involve different processes as well as much higher energies, and should not be confused with ordinary novae.