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The dependence of scintillation caused by equatorial bubbles on the electrondensity in the post sunset anomaly cannot generally be determined becausethe irregularities that produce the scintillation obscure the measurement ofthe electron density. This work addresses this problem with the introductionof a new technique based on the finding that anomaly electron density is soregular that its LT distribution can be fit by a polynomial over itspost-sunset extent. By means of this polynomial, gaps in the data caused bythe irregularities can be inferred where otherwise not measurable.Observations are of amplitude scintillation at 1.5 GHz from the Marisatsatellite and of NmF2 measured by ionospheric soundings at Ascension I. inMar 2001 during solar maximum. The result is that the well defined maximumof the S4 scintillation index is a linear function of coinciding NmF2.Evidence that supports this result has been found in 3 differing cases: Thefirst finds that both S4 and NmF2 decrease linearly with LT; the second,that both occurrence of scintillation and NmF2 increase linearly with F10.7cm solar flux; the third finds a linear relation between occurrence ofscintillation at 137 MHz and NmF2. The importance of these results is thatscintillation is caused by the bubble, but its magnitude is determined bythe magnitude of the electron density that the bubble intersects. A furtherimplication is that, given the unpredictability of bubbles, if NmF2 could bepredicted, the maximum level of S4 possible could be predicted if a bubblewere to occur

The linear dependence of GHz scintillation on electron density observed in the equatorial anomaly