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O'Connell Effect
The way this program works is it starts by asking if you have 1-3 file filters (Johnson B, Johnson V, and/or Cousins R) and then asking for an Epoch, period, and the output file path location. Once these things have been entered, the program goes on to calculate various values of the O'Connell Effect based on this paper https://app.aavso.org/jaavso/article/3511/.
The program outputs a table for all the O'Connell effect values for each filter that the user enters and a figure with all filters in the top panel with a synthetic fit. The lower panel shows the residual line of the data given that synthetic fit.
More specifically, the program calculates various Fourier fit coefficients, OER, and LCA.
Where OER is defined as the ratio of the total area under the curve between phases 0 and 0.5 over the phases 0.5 and 1. Given a ratio of 1 there is no O'Connell effect and an OER over 1 implies that right half of the light curve has more total flux than the left.
LCA measures the deviance from symmetry of the light curve and a LCA of 0 implies no O'Connell effect.
If a_1 is 0 then the system can be implied to be symmetrical. To determine if a star is either a W UMa or a Beta Lyrae, you can see if a_4 > (0.125 - a_2). Then if this condition is met, then see if |a_1| < 0.05. If this condition is met, you can assume the system is a W UMa.