The Coherent Radio Emission from the RS CVn Binary HR 1099
O. B. Slee A , W. Wilson A and G. Ramsay APublications of the Astronomical Society of Australia, 2008, 25, pp. 94–104
Publications of the Astronomical Society of Australia 25(3) 154-154 https://doi.org/10.1071/AS07045_CO
Published: 29 September 2008
Section 2.2 should be replaced with the following text.
2.2 Analysis of High Time-Resolution Data
Our analysis of the high time-resolution data was intended to elucidate the temporal structure of the highly polarised emission. We did this by allocating the data to six bins containing the samples integrated over 40, 10, 2.5, 0.625, 0.156 and 0.078 s and then finding the average Stokes V intensity in each bin. Call the mean flux density associated with each bin, 
St
, say, and its variance σt
2, where t signifies the integration time of samples assigned to that bin. In addition, the ith individual flux density in that bin has its residual mean square value, σi
2, which is dependent on the system noise and will also make a contribution to σt
2. Therefore, to compute the variance due to the star’s intensity variability between samples in the bin, στ/
2, we have:
in which the σι have been averaged over all the samples in the bin.
The rms value of the stellar variability is thus;
Next, to assign a meaningful measure of this variability, we define a modulation index:
