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However, the 10.17ish from that paper seems to be just the contribution from the Red Giant star in the binary, and what we measure should be the combined flux from the entire binary system including the accretion disk. At the moment, from the AAVSO light curves, I would think a Vmag of 9.8 (fluctuating between 9.75 and 9.85 perhaps) should be about right. If we assume those values and no variability of the donor on short timescales (hours), if my math is right, it would mean that the accretion disk alone, without the red giant donar star, fluctuates between roughly 11.0 mag (V) and 11.3 mag (V) on short timescales, right?
I have now used my little tool to evaluate the brightness of T CrB in real-time with a Seestar S50 smart telescope (and sound an alarm to wake me up in case of an outburst!) for more than 20 clear nights, some with rather challenging intermittend clouds) and I’m now confident enough to recommend its use by others.
https://github.com/Bikeman/SeestarPhotometricWatchdog
I still need to correct many typos in the documentation files README.md and Adv_Documentation.md (which were written in a frenzy to outrun T CrB going nova…) but the scripts themselves are stable.
I’m still looking for people who want to give this a try with the newer Seestar S30 product. If someone wants to port this to Windows, that would also be most welcome (it’s currently intended to be hosted on a Raspberry Pi or other Linux host).
CS
HBEIs the Symbiotic Recurrent Nova T CrB Late? Recent Photometric Evolution and Comparison with Past Pre-Outburst Behaviour
I hoped they may stick their necks on in the section 4.3 “when will T CrB erupt?”. They observe that “Recent photometric and spectroscopic observations indicate that the system is returning to a high-accretion state. Given this, an eruption may be imminent, even without distinct precursors”. So, as ever, we shall just have to keep on watching as there might be no warning.
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