No abstract

We analyze $V$-band photometry of the aperiodic variability in T CrB. By applying a simple idea of angular momentum transport in the accretion disc, we have developed a method to simulate the statistical distribution of flare durations with the assumption that the aperiodic variability is produced by turbulent elements in the disc. Both cumulative histograms with Kolmogorov-Smirnov tests, and power density spectra are used to compare the observed data and simulations. The input parameters of the model $R_{\rm in}$ and $\alpha$ are correlated on a certain interval and the most probable values are an inner disc radius of $R_{\rm in} \simeq 4 \times 10^9$ cm and a viscosity of $\alpha \simeq 0.9$. The disc is then weakly truncated. We find that the majority of turbulent events producing flickering activity are concentrated in the inner parts of the accretion disc.Comment: 9 pages, 10 figures, accepted for publication in MNRA

Abstract. We have combined recent radial velocity measurements of Fekel et al. (2000) with previously studied older ones, to test for the continued presence of the second period, found by Gális et al. (1999), which could be due to pulsations of the cool component of the AG Dra binary system. Fekel's data, even taken by themselves, also marginally suggest the presence of variations near the previously found second period. The period is in any case clearly seen, when all radial velocity measurements are combined.