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Dear colleagues, I have tried, from spectra of different observers to find base lines of the Halpha emission components V & R out of eclipse. At least the peak heights of both seems to provide a good chance to determine the exact beginning of the eclipse. The dispersion of the measurements comes from the “natural” activities of mass transfer from the M2 super giant into the B star disk (EW & V/R variability). Comments are welcome!
Ernst
Jack, I’m preparing at present a plot of the time behavior of the peak height & equivalent width of the V and R component, in order to get a first impression of the baseline. The last measurement in that plot is from Februar 22th this year. So it would be great, if you could offer your spectrum soon to supplement the base line.
Ernst
Hi Marc, there is already an upload opportunity for VV Cep at the database. I think it’s not necessary to creat another one. Please send me your email adress for sending the ppt file. You can find my email adress at my website:
http://www.astrospectroscopy.de
Ernst
Hi Jack, I think every high resolved Halpha spectrum from now, will be a benefit for the campaign.
Ernst
Dear Marc, your possibilities to start at the beginning of May with high resolved observations sounds really good. I would be really happy, if you could contribute with such a kind of spectra. The more spectra we collect, the more precisely would be the estimation, of the time differences of the V and R eclipse. Probably I will be able to take my first spectra at the earliest in the middle of May. I designed an animation for an object related seminar in May at the University of the city of Wuppertal, in order to demonstrate in priciple the process of the eclipse. But unfortunately is not allowed to upload ppt files here. If you are interested, I could send it via email.
Ernst
Hi Steve, is there any chance for you, to use for VV Cep a spectrograph with higher resolving power? It would be so helpful for the observation of the eclipse of the Halpha components V and R !!
Ernst
Hi Andy, it would be really great if you could contribute with your spectra to that campaign. But you have to know, it will be fairly important to get a sufficiently long baseline before the eclipse of the V and R component, in order to determine precisely enough the intensity decrease of the emissions.
Ernst
Hi Andrew,
I think, the minimum resolving power should be around 12000. I don’t know your location, but at the beginning of August during midnight is the star near zenith and it should be possible to take spectra.
Ernst
Dear colleagues,
thank you for your cordially welcome.
I hope we will have interesting conversations about interpretation of spectra, physics of (Be) stars and its atmospheres.
Best wishes, Ernst Pollmann
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International Working Group ASPA
Active Spectroscopy in Astronomy
http://www.astrospectroscopy.de
https://bav-astro.eu/index.php/beobachtungspraxis/spektroskopie
