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Dear colleagues,
with the publication (link below) I would like to inform you about investigations of VV Cep.
Topic of the paper is the "Correlation of Halpha Emission flux with B & V magnitudes.
http://astrospectroscopy.de/media/files ... -print.pdf

The paper had to be revised. A new one is in progress.

Ernst Pollmann

Dear colleagues,
the correalation between Halpha EW and Vmag presented here, could be understand as confirmation of the wind accretion by the B companion as described in the paper above.
Thank you all for your continuing observation and sending of spectra. Ernst Pollmann

Dear colleagues !

Our ongoing investigation of possible connections between the visual brightness (Fig. 2) and the Halpha equivalent with (EW) (Fig. 1) does enable to communicate the following results:

1) the observed photometric Vmag variation does have its origin in the pulsations of the M supergiant, with a period of 145 days (see phase plot in Fig. 2)

2) In contrast to our earlier assumption of a physical correlation between the Halpha EW and the Vmag in Fig. 3, we have to say today that after the EW correction for the Vmag continuum there is no correlation (Fig. 4). We have to realize that we have more or less a constant line flux with a dispersion range of approx.10 Angstroems.

As conclusion of our investigations we can say, that the source of the Hα variability within the range of the accretion region around the hot companion (B star) is not linked with the pulsation period of the M supergiant, and that its causes remains further unclear. Best wishes, Ernst Pollmann
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International Working Group ASPA
Active Spectroscopy in Astronomy
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