Campaign Halpa RV of gamma Cas

Campaign Halpa RV of gamma Cas

Postby Ernst Pollmann » Sun Jun 28, 2015 9:37 am

Dear colleagues,
as you already know, several ARAS observers take part successful at the Halpha RV campaign, in order to determine the orbital eccentricity in the sense: zero or not zero (that's here the question).
At present we are on the ascending RV branch, and it would be great, if further observers could contribute with high-resolution spectra (for example LHIRES, 2400) to that campain.

Best wishes, Ernst Pollmann
---------------------------------------------
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Active Spectroscopy in Astronomy
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Re: Campaign Halpa RV of gamma Cas

Postby Ernst Pollmann » Sat Oct 03, 2015 3:52 pm

Dear colleagues,
here an information about the current observation state of the campaign.

Ernst Pollmann
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Re: Campaign Halpa RV of gamma Cas

Postby Ernst Pollmann » Thu Oct 22, 2015 2:26 pm

Dear colleagues,
I would like to inform you about the ongoing monitoring of the radial velocity of gamma Cas.
Particularly the continuous observations of Patrik Fosanelli, emphasizes the (un-expected) second distortion (this time) in the descending branch of the velocity curve. I will inform our professional partners (A. Miroshnichenko & M. Smith) about that phenomenon.

Ernst Pollmann
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Re: Campaign Halpa RV of gamma Cas

Postby Ernst Pollmann » Sat Jan 23, 2016 9:22 am

Dear colleagues,
herewith I would like to inform you (particularly A. Wilson, T. Lester, P. Fosanelli, M. Schwarz, C. Sawicki, J.N. Terry, P. Berardi, Th. Lemoult because of their current BeSS spectra) about the current RV characteristics of gamma Cas.
My impression is that the RV scatter became larger (caused by further disk re-structuring) since the last maximum around JD 2457250.

Ernst Pollmann
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Re: Campaign Halpa RV of gamma Cas

Postby Ernst Pollmann » Thu Sep 06, 2018 3:45 pm

Dear colleagues!
For a certain reason I want come back to the importance of the observation of the Halpha radial velocity in gamma Cas (see postings above).
Even if some observers believe, that it would be not necessary to observe frequently this "well known" (?) Be binary star, there are phenomenons in its radial velocity which required exactly the opposite.
We found at a certain time an irregularity in the sinusoidal course of the RV, which our professional consulters interpreted as indicator of a changes in the morphology of a no longer perfectly axis-symmetric disk. See the attached comments of the experts Dr. Myron Smith and Prof. Dr. Anatoly Miroshnichenko.
Report to ARAS.png
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And when we receive ideally one spectrum/day, then we would be able in case of the repetition of our earlier observation to judge, whether it is a real disturbance in RV, or observation errors.
In that sense I want to encourage all interested Be star observers, not to neglect observations of this system, in a high spectral resolved mode.

Ernst Pollmann
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