[vsnet-chat 464] V1974 Cyg, CP Pup, V603 Aql & RW UMi progenitors

[Alon Retter <alon@wise1.tau.ac.il>]

> From tkato@kusastro.kyoto-u.ac.jp  Thu Jul 24 05:16:16 1997
> To: vsnet-chat@kusastro.kyoto-u.ac.jp
> Subject: Re: V1974 Cyg and CP Pup progenitors - answer to Taichi Kato
> 
> Dear Dr. Retter,
> 
>     According to Warner's "Cataclysmic Variable Stars", CP Pup was reported
> to be fainter than mag 17 before eruption (Gaposchkin 1946 = Harv. Coll.
> Obs. Bull. No. 918).  It would be interesting to check this source reference
> (missing here!).
> 
>     Warner also lists pre- and post-eruption magnitudes of three very fast
> novae.  From his Table 4.5:
> 
>           Porb      mv(max)  mv(pre)  mv(post)
> GQ Mus    1.43 hr      7       >21      17.5
> CP Pup    1.47         0.2     >17      15.0
> V1500 Cyg 3.35         1.8     >21      17.2
> 
>     I think RW UMi is another example of novae which stick in brighter
> post-eruption magnitudes than pre-eruption ones.
> 
> Regards,
> Taichi Kato
> 
------------------------------------------------------------------------
Dear Dr. Kato,

Thank you very much for this answer. I will try to get this old
paper of Gaposchkin. It is Geology and not Astronomy!

As for RW UMi, it is indeed about 2 mag. above its preoutburst
level, but the nova decayed first to its 21st pre-discovery mag.,
and the light was increased afterwards. (Howell et al. 1990, PASP,
102, 758), so it's probably a different case.
It is intereting to note that Howell et al. 1991, PASP, 103, 300
suggests an orbital period of about 2 hr, that fits a superhumps
interpretation, but the run was only 3hr.

I wander whether anyone can comment on the progenitor of V603 Aql.
Is it known? Is it below its mv=12 present state?

Greatings
Alon Retter

VSNET Home Page

Return to Daisaku Nogami

---

vsnet-adm@kusastro.kyoto-u.ac.jp