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Yes that is a a copy of the IAUC with a request for observations. (confusingly that IAUC covers several diverse object discoveries)
“Could the difference be epoch 1950 for the IAU notification as opposed to epoch 2000 for Simbad”
I was comparing with the FK4 (1950) coordinates for the object in SIMBAD
Cheers
Robin
The answer perhaps lies closer to home !
From VSSC #83 page 7
931207 LL And B.Marsden, CBAT, Paul Wild, Switzerland, Steve
Howell, USA, T.Kato, Japan, Bruce Margon, USA Object reported as a ‘nova’ in IAUC 3412 (1979) seen again in outburst by Tony Vanmunster, Belgium 1993 Dec 7 mag 14.Ov. Confirmed by Poyner. Kato obtains CCD images at Ouda on Dec 9 V=14.0. Suggests position needs correction. Howell obtains spectra and paper planned!
Robin
Tracked down the discovery IAUC. Difficult to say without knowing the precision of the coordinates given there but they could be up to ~1 arcmin away from the ones in SIMBAD for this star so not sure yet where the association comes from
Ah interesting. I see that paper suggested Oxygen might be found as well through the same process. One was found with just O in the spectrum, though by a suggested different mechanism where the He/H is stripped away.
https://physicsworld.com/a/white-dwarf-with-nearly-pure-oxygen-atmosphere-surprises-astronomers/
I see this has now faded to Vmag ~15 so time for perhaps a last low resolution spectrum. It shows a nebula type spectrum with strong forbidden emission lines, particularly [OIII] and a very weak almost undetectable continuum (The Y scale is relative to the continuum at 5500A and the signal/noise in the continuum is down in single figures). In fact I estimate 78% of the light in the V passband comes from just the [OIII] pair of lines at 4959/5007 A
A quick literature search though brought up this reference which talks of WD with initial He atmospheres evolving an H dominated atmosphere through upward diffusion of H.
https://arxiv.org/abs/2008.07469
Anything heavier though I suspect must have been accreted.
I don’t know how it relates to the progenitor but as I understand it, naked electron degenerate white dwarfs don’t show any spectral features and there are indeed some WD like that, designated spectral type DC. The spectral features then come from a thin skin of accreted material, the heavier elements rapidly sinking into the interior to become part of the electron degenerate material so most show just H while others have He or a mix of H/He. You do also find some cool white dwarfs with Carbon in their spectrum, presumably also recently accreted.
Yes it was already clear in 2019 😉
The OI 7774 line is possibly there under the 2nd order but out of focus
Now at mag 16 but still within range of a very low resolution spectrum with the ALPY200.
The spectrum with several forbidden nebula lines looks similar to that of another very fast nova Sgr 1991 at similar age in Gray & Corbally , where the tentative line identifications come from
Cheers
Robin
“ (is a 50% increase in effective radius due to pulsations feasible?)”
Though of course a smaller change in radius would be sufficient depending on the path of the hot star behind the M star
Yes I agree. If the continuous brightness variations are due to radial pulsations of the M star, these would produce changes in the effective radius (and opacity?) of the M star. These could could asymmetrically shift the mid eclipse point dependent on their timing. (is a 50% increase in effective radius due to pulsations feasible?)
Cheers
Robin
Hi Andy,
The measurements pre 1997 were all based on the light curves which are indeed tricky to estimate the mid eclipse point from due to the continuing brightness variability of the red giant throughout the eclipse seen in the AAVSO data in fig 5 of Hugh’s paper. The photometry and spectroscopy were in good agreement within 7 days in 1998 though.
I have extracted B-V from the AAVSO data which is less influenced by brightness variations than using using V I think. I have marked Hugh’s spectroscopic mid eclipse and the expected values based both on the earlier ephemeris and assuming a 60 day increase in period post 1978.
Hugh’s value agrees well with the B-V data. The prediction based on a permanent increase in period is clearly not compatible with the current data but perhaps there is enough wriggle room to say that the original ephemeris is ok and the 1997-1998 eclipse data (both spectroscopic and photometric) was anomalous for some reason?
Cheers
Robin
The argument for something to have happened though between 1978 and 1998 is convincing from fig 4 of the 1999 Graczyk et al paper if the error bars are to be believed
There is an absolutely stunning high resolution echelle spectrum covering 3750-9300A in the BAA database from Joan Guarro Flo taken 20210809.838 using an amateur designed (by Tim Lester) home built remotely operated instrument. (zoom in to view the narrow P Cygni lines from the stellar wind superimposed on the broad nova ejecta lines) An impressive example of the progress in amateur spectroscopy since the last outburst.
Cheers
Robin
“The narrow unshifted feature comes from the circumsystem material from previous outbursts”
Correction that should be ….from interaction with the relatively slow moving red giant wind. This looks a good reference for the evolution of the optical spectrum in the 2006 outburst
https://academic.oup.com/mnras/article/474/3/4211/4768437
Robin
This is only the start! (The narrow unshifted feature comes from the circumsystem material from previous outbursts). If it follows earlier outburst there is lots more strangeness to come. Watch for highly ionised coronal lines (like [Fe X, XI, XIV] and [A X] etc) produced as the shock heats the gas to 1 million K plus. There is an interesting account of taking spectra early in the 1958 outburst by George Wallerstein in the 2005 S&T article.
Robin
A series of spectra from 2006 taken using a Star Analyser.
http://www.threehillsobservatory.co.uk/astro/spectra_24.htm
I expect there will be many more spectra this time
Cheers
Robin
