Recently, we have investigated the photometric history of the hot S Dor type stars, or Luminous Blue Variables (LBVs) AG Car, S Dor and

Car comprising over a century of photometric observations (van Genderen et al. 1996, hereafter called Paper I; de Groot et al. 1996). We proposed that the S Dor (SD) activity is caused by two types of SD phases: the very long-term (VLT-SD) and the normal SD phases. The latter are superimposed on the former. Since in the visual maxima the mass-loss rate is generally not much higher than during the minima (e.g. de Koter et al. 1996), one should not call the light maxima "SD eruptions'', but rather "SD phases''. In the present paper we investigate the photometric histories of five other LBVs, although the time intervals over which the stars were well monitored are generally much shorter than a century. We attempt to categorize the various long- and short-term light and colour variations.

**Table 1:** List of data sets and the type of photometry. For HR Car bracketed abbreviations are used in Fig. 1 (click here)

Star	Type	Reference/Group	Remarks
HR Car	pg	Hoffleit (1940) (H pg)	1
	VBLUW	Graham (1968) (Gh )	2
	UBV	Bond & Landolt (1970) (BL )
	UBV	Wisse & Wisse (1971) (WW )
	VBLUW	van Genderen et al. (1990) (vG et al. )	2
	VBLUW	unpublished, made in 1990 (vG et al. )	2
	vis	Bateson (1987-1990) (Ba mv)	3
	vis	AFOEV (A mv)	4
	uvby	LTPV (LTPV )	5, 6
	uvby	Kilkenny et al. (1985) (K et al. )	6
	Geneva	(G, )	6, 7
R127	uvby	LTPV	5, 8
	VBLUW	unpublished, made in 1983, 1986-1990	2
	various		9
R40	uvby	LTPV	5, 10
	VBLUW	unpublished, made in 1987-1989	2
	various		11
R71	VBLUW	van Genderen (1979)	2
	VBLUW	van Genderen et al. (1985, 1988)	2, 6
	VBLUW	unpublished, made in 1988 and 1989	2
	uvby	LTPV	5, 6
R110	VBLUW	Walraven & Walraven (1977)	2, 12
	various		13
	uvby	LTPV	5
	VBLUW	unpublished, made in 1989-1991	2

Remarks to Table 1 (click here):
¹ The 700 estimates were averaged by her about each 200d and given in the international magnitude system.
² Walraven V transformed into

of the UBV system.
³ Shown as a smooth curve by Hutsemékers & van Drom (1991).
⁴ Association Française des Observateurs d'Etoiles Variables. Scatter amounting to

01 in the maxima and

03 in the minima, but the observations are represented by a smooth curve.
⁵ Observations made by the observers of the Long-Term Photometry of Variables project organized by Sterken (1983) and published by Manfroid et al. (1991, 1994) and Sterken et al. (1993, 1995). Note that

.
⁶ For a first discussion (of part) of these observations see Spoon et al. (1994).
⁷ Observations made by the Geneva observers. Geneva V close to

of the UBV system.
⁸ The following data were rejected because of their unexplainably large deviations

, 7405.914, 7468.730, 7477.621, 7480.617, 7777.877, 7792.840, 7825.682, 7836.741, 8099.930 and 8255.616. It is possible that the observers erroneously observed the nearby star R128 = HDE269859, or that the close optical companion HDE269858p (2

), also a supergiant in the LMC, is variable as well.
⁹ Observations in various photometric systems, if necessary transformed to

, based on the work by Stahl et al. (1983), de Groot (quoted by Stahl et al. 1983) and van Genderen (1970).
¹⁰ Observations in the u passband rejected because of their peculiar values: JD9292.7248, 9292.6728 and 9301.5615.
¹¹ Scattered observations collected from the literature by Szeifert et al. (1993).
¹² Made in the interval 1957-1963; only the average is given by them.
¹³ Observations in various photometric systems, collected from the literature by Stahl et al. (1984, 1990, those of Walraven & Walraven are mentioned separately in Remark 12), to which we added observations by Isserstedt (1975) made in the interval 1971-1973 and by van Genderen et al. (1982) made in October 1979.

1. Introduction