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[en] The cataclysmic variables are usually divided into the following four classes: novae; recurrent novae; dwarf novae, which are subclassified as U Geminorum stars or Z Camelopardalis stars; and novalike variables. Those observations that bear most directly on the structure of cataclysmic variables at minimum light are reviewed. Sections include: the basic model; masses; the structure of the disk; the rapid oscillations; and the source of the eruptions. 5 figs., 4 tables, 133 refs

[en] A catalogue of all published preeruption photometry of novae is presented, and preeruption light curves are constructed for 11 of the stars. With the possible exception of BT Mon, the preeruption and posteruption magnitudes are the same for all 18 stars for which both magnitudes are known. Twelve stars have well-defined preeruption light curves. Six of the 12 show changes in their light curves in the 1-15 yr prior to their eruption. Five of the six stars show a rise in brightness by 0.25 to 1.5. None of the available theories of the nova eruption can account for this preeruption rise. RR Tel became a long-period regular variable prior to its eruption. It is argued that the behavior of RR Tel suggests that the M5 III star in the binary must control the eruption. The preeruption and posteruption light curves of one star, V446 Her, are different. The prenova varied irregularly by almost 4 mag. The postnova does not vary by more than 0.4. (auth)

[en] Characteristics of pulsating white dwarf stars are discussed. The ten known pulsating white dwarfs are listed along with their color characteristics

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No abstract available