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(fwd) query on PNe and pre-CVs
The following message is from Gunter Cibis. Since the raised questions
and listed information are of public interest, I forward them to this list
(Gunter Cibis is already on this list, so please fell free to post any
comments or replies to the list).
From: "Gunter Cibis" <gunter@cibis-nt.de>
Subject: planetary nebulae and cataclysmic variables
Date: Sun, 8 Jun 2003 19:14:44 +0200
Dear Dr. Kato,
Please allow me to contact you again. I know I put many questions, but the subject is very interesting.
Your answer is very important for me. I promise I will disturb you not too often.
Some cataclysmic variables seem to be related to planetary nebulae (PN):
The spectrum of the central star of HFG 1 (PN G136.3+05.5) (V664 Cas) shows characteristics of a
cataclysmic binary (Acker and Stenholm 1990).
The spectrum of the central star of A 65 (PN G017.3-21.9) closely resembles that of a cataclysmic
binary. One other confirmed PN also has a similar spectrum - HFG 1 (Walsh and Walton 1996).
The object 0623+71 seems to be a PN and not a shell resulting from a nova outburst (Krautter et al.
1987). PG 0623+71: cataclysmic binary nucleus surrounded by a PN (Bond 1989). The PN
designation is EGB 4 (PN G143.6+23.8) (Ellis et al. 1984).
Is PG 0623+71 indeed a cataclysmic binary nucleus ?
UU Sge, the Algol-type eclipsing binary central star of A 63 (PN G053.8-03.0) ultimately will become
a cataclysmic variable (Bond et al. 1978).
Do you share the opinion that UU Sge ultimately will become a cataclysmic variable ?
If yes, which timescale can we estimate ?
The Algol-type eclipsing binary V477 Lyr is the central star of the PN A 46 (PN G055.4+16.0).
Will V477 Lyr also ultimately will become a cataclysmic variable ?
If yes, which timescale can we estimate ?
BE UMa is a precataclysmic binary system and planetary nebula central star (Liebert et al. 1995).
BE UMa is an Algol-type eclipsing binary.
Do you share the opinion that BE UMa is a precataclysmic binary system ?
If yes, which timescale can we estimate ?
Among several possible explanations of the origin of the hypersonic knots of MyCn 18 (PN G307.5-04.9)
is a recurrent nova-like ejection from the central binary star (O'Connor et al. 2000).
What do you think about the possible cataclysmic variable model for the central star of MyCn 18 ?
The observations of the old nova GK Per 1901 are interpreted in terms of an ancient planetary nebula
ejected from the central binary system (Bode et al. 1987).
There are severe problems with this interpretation (Tweedy 1995).
What do you think about the PN model for Nova GK Per 1901 ?
Barnard (1908) reported on variability (was it a dwarf nova outburst ?) of the central star of NGC 7662
(PN G106.5-17.6).
The variable star designation of the central star of NGC 7662 is NSV 14555 (Kohoutek 2001).
What do you think about the variability of the central star of NGC 7662 ?
Was it a dwarf nova outburst ?
The central star of A 35 (PN G303.6+40.0) (BD -22 3467 = LW Hya) is a binary system (e.g.
Jasniewicz and Acker 1988, Herald and Bianchi 2002). One component is a G8 IV star (e.g. Acker and
Jasniewicz 1990, Thevenin and Jasniewicz 1997). According to Jacoby (1981) one component is a
G8 III-IV star.
Observations of the central star of A 35 are interpreted as the behavior of a cataclysmic binary, where
one component is a Roche-lobe-filling subgiant star and the other a white dwarf surrounded by an
accretion disk (Acker and Jasniewicz 1990).
Thevenin and Jasniewicz (1997) showed for the G-type giant component of the central star of A 35
a photospheric enhancement of the barium element. The G-star could be a pre-barium star in a
detached binary system.
What do you think about the cataclysmic variable model for the central star of A 35 ?
Do you know more objects with a possible planetary nebula-cataclysmic variable connection ?
References
Acker, A., Jasniewicz, G.: 1990, Astron. Astrophys. 238, 325
Acker, A., Stenholm, B.: 1990, Astron. Astrophys. 233, L21
Barnard, E. E.: 1908, Monthly Notices Roy. Astron. Soc. 68, 465
Bode, M. F., Seaquist, E. R., Frail, D. A., Roberts, J. A., Whittet, D. C. B., Evans, A., Albinson, J. S.:
1987, Nature 329, 519
Bond, H. E.: 1989, IAU Symp. 131, 251
Bond, H. E., Liller, W., Mannery, E. J.: 1978, Astrophys. J. 223, 252
Ellis, G. L., Grayson, E. T., Bond, H. E.: 1984, Publ. Astron. Soc. Pacific 96, 283
Herald, J. E., Bianchi, L.: 2002, Astrophys. J. 580, 434
Jacoby, G. H.: 1981, Astrophys. J. 244, 903
Jasniewicz, G., Acker, A.: 1988, Astron. Astrophys. 189, L7
Kohoutek, L.: 2001, Catalogue of Galactic Planetary Nebulae, Abhandlungen aus der Hamburger
Sternwarte, Band XII
Krautter, J., Klaas, U., Radons, G.: 1987, Astron. Astrophys. 181, 373
Liebert, J., Tweedy, R. W., Napiwotzki, R., Fulbright, M. S.: 1995, Astrophys. J. 441, 424
O'Connor, J. A., Redman, M. P., Holloway, A. J., Bryce, M., Lopez, J. A., Meaburn, J.: 2000,
Astrophys. J. 531, 336
Thevenin, F., Jasniewicz, G.: 1997, Astron. Astrophys. 320, 913
Tweedy, R. W.: 1995, Astrophys. J. 438, 917
Walsh, J. R., Walton, N. A.: 1996, Astron. Astrophys. 315, 253
I would be very pleased to receive an answer. It is nice that professional astronomers correspond with
amateur astronomers.
Thank you very much for helping. I wish you all the best.
With kind regards,
Gunter Cibis
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