The emission-line variable HBV 475.

Stienon, F. M.; Chartrand, M. R.; Shao, C. Y.

doi:10.1086/111529

Cited by 14 publications

(14 citation statements)

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“…Their adopted period for the light minima, which includes both pre-and postoutburst determinations, is 956.5 days, essentially identical with the result given in Stienon et al (1974). From their analysis of spectropolarimetry Schild & Schmid (1997) found an orbital inclination of 86¡^2¡, conÐrming that V1329 Cyg is an eclipsing system.…”

Section: Discussionsupporting

confidence: 59%

“…He noted that there were some similarities to V1016 Cyg and that both stars could be members of the same class of objects. Stienon, Chartrand, & Shao (1974) presented the results of photographic and spectroscopic analyses. They determined photographic magnitudes from plates in the Harvard collection, as well as about three dozen more recent magnitudes from two other sources.…”

Section: Discussionmentioning

confidence: 99%

“…An analysis of the photographic observations revealed light variations with a period of 959^2 days. In addition, Stienon et al (1974) concluded that the sharply deÐned minima are probably the result of eclipses. Their examination of several objectiveprism spectra indicated that V1329 Cyg has spectroscopic characteristics in common with symbiotic stars.…”

Section: Discussionmentioning

confidence: 99%

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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: Discussionsupporting

confidence: 59%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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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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“…Pre‐outburst photometry suggests that V1329 Cyg has eclipses, or at least that it had them at that time. Stienon et al (1974) noted occasional 2.5‐mag dips in pre‐outburst photographic photometry and derived a period of about 959 d. Schild & Schmid (1997) analysed the same photometry, augmented with data collected by Kohoutek & Bossen (1970), and found nearly the same period from the dips. They had to ignore one data point that showed the binary to be faint when it should have been bright, but that could have been an unusually large negative fluctuation.…”

Section: Orbitmentioning

confidence: 93%

“…There are no star–star eclipses in post‐outburst observations, or at least none that are widely recognized, and no photospheric RVs to quantify orbital motion. 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.…”

Section: Overviewmentioning

confidence: 99%

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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The Peculiar Symbiotic Object V1329 Cygni: Single-Star Versus Binary Models

Grygar¹,

Chochol

1982

Astrophysics and Space Science Library

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The emission-line variable HBV 475.

Cited by 14 publications

References 0 publications

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

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

Variation mechanisms in symbiotic nova V1329 Cygni

The Peculiar Symbiotic Object V1329 Cygni: Single-Star Versus Binary Models

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