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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 (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 (4.55 KiB) Viewed 7968 times
- 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
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
Halpha
He I
He II
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) :
Christian Buil