Sun, 06/13/2021 - 12:46
Possible there are some observers, who are interested to contribute to a new long-term monitoring campaign of rho Cas. Attached is the Halpha RV and EW monitoring of the past combined with the newest state.
AAVSO Alert Notice 746 announces an observing campaign (spectroscopy, photometry, visual observations) on the yellow hypergiant rho Cas. Please see the notice for details and observing instructions.
There are threads for this campaign under the following forums:
- Campaigns and Observation Reports: https://www.aavso.org/rho-cas-campaign
- Spectroscopy: https://www.aavso.org/rho-cas
Please subscribe to these threads if you are participating in the campaign so you can be updated by the astronomer and by HQ. Join in the discussion or ask questions there!
Many thanks, and Good observing,
Elizabeth O. Waagen, AAVSO HQ
Are we observing Halpha exclusively or are there other regions of interest?
the first and primary aim of the campaign should be, to catch any possible ejections events as quick as possible and to document.
If we are successful in certain cases I suggest to take quick contact with the professional astronomy (A. Lobel et al., A. Aret et al., V. Klochkova et al.), they do have the corresponding analytical experience to suggest, what additional wavelenght regions should be monitored.
Monitoring of the ejection behavior of Rho Cas; Line flux and radial velocity of the Hα double peak emission
Our previous observation efforts to describe scientifically relevant radial velocities and emission fluxes in the Hα range do not seem to me from today's point of view and especially in view of our previous monitoring, to correspond to the research goals of professional astronomy.
According to Klochkova et al. we have also concentrated on the ejection process in the Hα range, because photospherical ejections are evidently particularly easy to detect in this spectral range. As before, our main focus is therefore still on the intensity behavior of the blue- and red-shifted Hα emissions, but now is supplemented by their radial velocity behavior (RV), which is why all the spectra provided by all observers involved in the Hα emission line profile have been re-evaluated. See: