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Figure 1: Light curves of the variables of our survey, except those stars already discussed in Lebzelter et al. (2005). Fourier fits with up to two periods are shown. Note that both axis scales vary from star to star. For A19, LW5, LW7, LW13 and LW14, a break has been introduced into the time axis for a better presentation of the light change. Errors on data points before JD2452700 are estimated to be 0.013 mag (Mount Stromlo data) while after this date the errors are estimated to be 0.007 mag (CTIO data). |
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Figure 2: Light curves versus phases for selected, monoperiodic variables from Table 1. The period given in the table was used to calculate the phase. |
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Figure 3: Colour-magnitude diagram of 47 Tuc. Variable stars are indicated by open circles. Asterisks mark stars taken from Fox (1982) while the triangle is V3 using data from Eggen (1975). For all variables mean magnitudes and colours were used. |
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Figure 4:
The K-![]() |
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Figure 5:
The tip of the 47 Tuc giant branch in the HR-diagram. K and J-K of the variables
were converted to log L/![]() ![]() ![]() ![]() |
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Figure 6:
The K-![]() |
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Figure 7:
Luminosity L, pulsation period P and radii of several mass points
plotted against time in a model with
M = 0.6567 ![]() ![]() |
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Figure 8:
The growth rate
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