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tokens: short ones (lasting a few days) and superoutbursts, which can last two weeks or longer in their rather bright ‘plateau’ phase. Typical superoutburst cycle lengths of these ‘ordinary’ SU UMa stars range from 100–500 d. Two additional subgroups can be distinguished: WZ Sge stars have longer superoutburst cycle lengths (several thousand days) and lack the normal short outbursts, while ER UMa-type dwarf novae are characterized by very short superoutburst cycles (20–40 d), and even more frequent normal outbursts in between. More than four decades ago, periodic ‘superhumps’ were detected in the SU UMa star VW Hyi (Vogt 1974 ; Warner 1975 ) during a plateau phase; later they turned out to be a characteristic feature of all SU UMa stars, but they also appear occasionally in other CV types, as classical nova remnants and nova-like stars (Patterson 1999 ). Since then, and till now, most observational efforts on SU UMa stars have been concentrated on the detection of superhumps and the determination of their properties (Kato et al. 2017 and the previous papers of that series), widely neglecting the systematic coverage of the general outburst behaviour of these and other dwarf novae. The semiregular outburst behaviour of DNe has attracted the interest of amateur astronomer societies for a long time, such as the American Association of Variable Star Observers (AAVSO), the British Astronomical Association (BAA), and the Royal Astronomical Society of New Zealand, Variable Star Section (RASNZ, VSS), and very valuable long-term light-curve studies have already been published decades ago, containing catalogues of individual outbursts with their main properties as maximum brightness, amplitude, width, and classification according to light-curve shape, as well as some statistical analyses of these properties. As typical examples, we can mention here extensive studies on SS Cyg (Mattei, Saladyga Waagen 1985 ), U Gem (Mayall 1957 ; Mattei et al. 1987 ), and VW Hyi (Bateson 1977 ). To our knowledge, no long-term studies like those of the 1960s and 1970s have been published more recently. Simultaneously, there was and still is a boom in the number of detections of new CVs, especially dwarf novae. The VSX AAVSO catalogue (Watson 2006 ) lists more than 9000 DNe, but does not give any cycle length information. The latest online version of the CV catalogue of Ritter Kolb ( 2003 , version 7.24, 2017 February) list a total of 852 DNe with known orbital period, 631 of them (74 ) classified as SU UMa, ER UMa, or WZ Sge stars. Only for 121 (19 ) are some cycle length data given. Discounting the doubtful cases, Ritter Kolb ( 2003 ) give, for a total of only 73 cases (12 ), reliable information on the lengths of the superoutburst cycle (hereafter ‘supercycle length’). However, no references are given for the cycle lengths, and it is often very difficult and time-consuming to check these data. Therefore, we here determine supercycle length values of other SU UMa stars, for which