The possibly massive symbiotic system V 1329 Cygni

Iijima, Takashi; Mammano, A.; Margoni, R.

doi:10.1007/bf00648640

Cited by 24 publications

(23 citation statements)

References 12 publications

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“…ments of this orbit for the hot component based on visual lines can be found in Iijima, Mammano, & Margoni (1981) and Chochol & Vittone (1986). However, from several lines of argument Baratta & Viotti (1990) concluded that those emission-line velocities do not represent the orbit of the hot companion.…”

Section: Discussionmentioning

confidence: 99%

Infrared Spectroscopy of Symbiotic Stars. III. First Orbits for Three S-Type Systems

Fekel

Hinkle

Joyce

et al. 2001

The Astronomical Journal

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Infrared radial velocities have been used to derive the Ðrst well-determined orbital elements for the cool giants of three symbiotic systems, BF Cyg, V1329 Cyg, and V343 Ser\AS 289. Periods found for BF Cyg and V1329 Cyg from the radial velocity data are in good agreement with periods previously determined for their light variations, and the orbits are circular. Masses for the components of BF Cyg and V1329 Cyg were determined by combining our orbital elements for the cool giants with elements for their hot stars. BF Cyg and V1329 Cyg are shown to be detached binary systems. The third system, V343 Ser, has an orbital period of 450.5 days, a value that is typical for symbiotic binaries. However, the system is atypical because of its somewhat eccentric orbit, with e \ 0.135 and the possibility that it is a semidetached system. An orbital inclination of 18¡ is estimated, indicating that V343 Ser does not eclipse.

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Section: Discussionmentioning

confidence: 99%

Infrared Spectroscopy of Symbiotic Stars. III. First Orbits for Three S-Type Systems

Fekel

Hinkle

Joyce

et al. 2001

The Astronomical Journal

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“…However Andrillat (1973), Mammano & Righini (1973), Stienon, Chartrand & Shao (1974) and Hric, Chochol & Grygar (1978) established that V1329 Cyg is a two‐temperature source and a symbiotic binary. There are emission line RVs also (Grygar et al 1979; Iijima, Mammano & Margoni 1981, hereafter IMM81; Tamura 1989; Ivison, Bode & Meaburn 1994; Nussbaumer, Schmutz & Vogel 1986, hereafter NSV86; this paper) that suggest orbital motion when averages are taken over many lines. Those lines appear to be associated with the blue star but are not actually from that star.…”

Section: Overviewmentioning

confidence: 96%

“…The RVs formally yield non‐zero estimates for eccentricity ( e ) that might possibly be meaningful (e.g. IMM81; Chochol & Vittone 1986; NSV86; this paper), although the reality of the derived e and argument of periastron ( ω ) is difficult to judge because various ions give different RV curves. The disagreements may arise from the individual line velocities being influenced by turbulent sub‐region motions and therefore not corresponding to blue star velocities, except perhaps roughly on average.…”

Section: Orbitmentioning

confidence: 99%

“…The names should not be taken too literally, as the early and late sets overlap considerably in time and the statistics are not good enough to establish clearly whether time or some other discriminant is responsible for their distinct behaviours. The early set runs from about JD 244 0500 to JD 244 6400 and contains 28 averaged points from table IV of IMM81, 21 points from Tamura (1989), 14 points from Grygar et al (1979), plus 15 He ii points and 15 C iii points from table 6(a) of NSV86 (the points labelled ‘v1’ by NSV86). The late set spans about JD 244 4000 to JD 244 9000 and contains the data of this paper listed in Table 1 plus 12 observations by Ivison et al (1994).…”

Section: Orbitmentioning

confidence: 99%

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Variation mechanisms in symbiotic nova V1329 Cygni

Chochol

Wilson

2001

Monthly Notices of the Royal Astronomical Society

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U, B, V light curves of symbiotic nova V1329 Cygni (=HBV 475) are modelled in terms of combined wind and chromospheric fluorescence, with eclipses and shadowing of fluorescent regions, eccentric orbit effects, and conversion of far‐ultraviolet energy into the optical bands. Observational evidence regarding fluorescent brightness variation mechanisms is provided by waveforms and amplitudes and their changes from bandpass to bandpass. The combined set of U, B, V variations cannot be satisfied with a wind‐only or chromosphere‐only model. Contrary to arguments in the literature, chromospheric fluorescence can be comparable to wind fluorescence in brightness and can be far stronger than photospheric emission from a red giant. We show why there is no conflict between the existence of strong chromospheric fluorescence and symbiotic binary energetics, at least in this example. Ultraviolet and optical radial velocities are also discussed and fitted. Some parts of the fluorescent binary model omitted from the original paper by Wilson for lack of space are given here. Fitting was done both subjectively and by differential corrections (least‐squares criterion), thus providing insight into the interplay of wind and chromospheric effects. The large bandpass‐dependent waveform and amplitude changes are accounted for by differing relative amounts of wind and chromosphere fluorescence, with the chromosphere relatively bright in U and the wind relatively bright in B and V. A strong test of the model is provided by the way the amplitude and waveform change together – larger amplitude must go with wider minima, as observed. The differential corrections solutions fit the light curves rather well. Because they were done in JD rather than in phase, the solutions were also able to find ephemeris parameters. Potentially interesting is an enormous period change of dP/dt≈−0.0020±0.0004 s.d. which, if confirmed, means that the ≈955 d period is dropping by 2 d each cycle. Parameter results are tabulated, but our emphasis is on identification of variation mechanisms rather than specific numbers. Observational selection favours discovery of periodic fluorescent variation for arguments of periastron near ω=π/2 because wind and chromospheric fluorescence then combine to give maximum amplitude. The possibility of pre‐outburst drops in brightness being eclipses is examined. We urge spectroscopic observers to gather infrared radial velocities of the red giant and to search for subtle evidence of eclipses of the hot object. Infrared light curves also would be helpful if reasonably large numbers of data points could be accumulated.

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“…Indeed, the observation of intense forbidden lines indicates the presence of a diluted, highly ionized medium near or around the symbiotic object. Strong high-ionization lines (HeII, NIII, [OIII], [NeIII], [NeV], [FeVII]) have, in fact, been identified in the spectra of many symbiotics, and have long since raised the problem of their origin, e&, whether collisionally or radiatively ionized (for instance, Ilowaisky and Wallerstein, 1968). Of particular interest is the intriguing problem of the still unidentified broad features at 6830 and 7088 A.…”

Section: Vc the Optical Emission Line Spec-trummentioning

confidence: 99%