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Re: AG Dra brightening

Posted: Sun Jun 12, 2016 4:46 pm
by Francois Teyssier
Update of Raman OVI equivalent width
The V curve in green (inversed scale)
AGDra_OVI.PNG
AGDra_OVI.PNG (7.87 KiB) Viewed 7986 times

François

Re: AG Dra brightening

Posted: Sat Jun 18, 2016 10:07 am
by umberto sollecchia
Bonjour à tous, voici ma contribution à cette symbiotique .
Profilo AG Dra.png
Profilo AG Dra.png (4.55 KiB) Viewed 7968 times
Comparison.png
Comparison.png (5.02 KiB) Viewed 7966 times
Sincèrement.
Umberto

Re: AG Dra brightening

Posted: Sun Jul 17, 2016 4:40 pm
by Joan Guarro Flo
AG Dra, in the night 2016 07 16.
J. Guarro

Re: AG Dra brightening

Posted: Sat Apr 08, 2017 9:08 am
by Joan Guarro Flo
Hi,

AG Dra on the night 2017 04 07.

Cheers, Joan.

Re: AG Dra brightening

Posted: Mon Apr 10, 2017 4:05 pm
by Francois Teyssier
A full commented spectrum, using Tim's PlotSpectra
Taken during last outburst (cool outburst), so Raman OVI very weak
agdra_20160423_890_commented.png
François

Re: AG Dra brightening

Posted: Mon Apr 10, 2017 7:17 pm
by Forrest Sims
Here is a commented (ignoring the Balmer lines to reduce clutter) spectrum using PlotSpectra of AG Dra from last night. Maybe someone could enlighten me on the significant lines to look for and how to interpret the strength or weakness of these lines as compared to François spectrum in outburst?
Thanks!
Forrest

Re: AG Dra brightening

Posted: Tue Apr 11, 2017 1:10 pm
by Christian Buil
Part of a VHIRES-MO spectrum (R=48000) + C11 telescope taken last night:

Raman O IV

Image

Halpha

Image

He I

Image

He II

Image

Christian Buil

Re: AG Dra brightening

Posted: Tue Apr 11, 2017 2:11 pm
by Francois Teyssier
Hi Woody

The giant of AG Dra is a K0-K3 giant of low metallicity. This is the reason why Fe lines do not appear

At low resolution, what can we do?

Measure Hb and HeII 4686
Let K = 0.534 * F(HeII)/F(Hb)
The temperature of the hot object can be estimated: T = 19.38*K^1/2 + 5.13 (in 10000 K unit)
This is a simplified Iijima's formula (1981), derived from Zanstra method

The ratio between HeI singlets and triplets (for instance 6678 and 5876) is a valuable indication of the electronic density

The flux of Raman OVI lines 6830 7085 (Raman scattering of O VI λ1032, 1038 A photons off neutral hydrogen) allows amateurs to "see" the farUV
The évolution of the flux of these lines will depend of the type of outburst ("cool" : they will nearly desappear "hot" : remain bright)
Interesting : the ratio F(6830)/F(7085). See Shore &al. (2010) : https://arxiv.org/abs/0912.1890

At higher resolution : lines profiles, radial velocity of the RG, ratio between the bue and red part of Raman OVI lines ...

Look at: http://www.astronomie-amateur.fr/Docume ... CE2016.pdf


All the best

François

Re: AG Dra brightening

Posted: Sat Apr 15, 2017 11:09 am
by Christian Buil
Comparison of 11/04 and 14/04 observations of AG Peg (Halpha). No very significant variation (the telluric are removed for a better comparison) :

Image

Christian Buil