Hi Ernst,
Thank you for looking at it! Actually I don't contradict to your theory here:
"...then the variations in your spectra does not contradict at all the "theory of the disk variability""
To be more precise, my statement is: my spectra show contradiction with a possibility, that the most of H11 would come from a B disk's emission. (Same applies to H10.)
Because if it would, we wouldn't see both R and V wings still prominent, once after B went into eclipse:
It is enough to know that the continuum part from B component dropped by 1.5 mag by now (see the already available Umag series) whilst M / B component ratio in this region was like 1/6 before the 1st contact, nowadays it should be like 1:1 very roughly (lower region, that's why not 1:2 that I measured for CaII). Some little continuum variation doesn't matter.
If H11 was mostly coming from a B star's disk, then both of its R and V wings should have been decreased a lot (as M continuum is coming up by a 2.5x factor), together with the B continuum.
The contrary has happened, V wing doubled and R wing remained prominent (see my graph above), well explainable by an external source (external from B), with a time coincidence by the eclipse event.
And, my +1 extra statement that it does have its own R/V variation - time is resolution is irrelevant here, I am not stating exactly what kind of variation it is or what's the period (still would be interesting to correlate the EWs with H-alpha). It is just rotating, that's clear to see.
Of course, some of the H-alpha variability (little or large portion: ?) may still be coming from a B star's disk. But, mostly not the H10-11.
Cheers,
Peter