Radial Velocity of the Central Star of NGC 1514

Mammano, A.; Margoni, R.; Perinotto, M.

doi:10.1007/978-94-010-3473-9_49

Cited by 3 publications

(4 citation statements)

References 1 publication

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“…1. Variations of the radial velocity for the central star were also reported by Mammano et al (1968) who observed a range from + 35 ± 10 to + 95±10kms _1 between 1965 and 1967. In Fig. 2(a) we show three of the five low-dispersion SWP spectra.…”

Section: Variabilitysupporting

confidence: 72%

The IUE Spectrum of the Binary Nucleus of the Planetary Nebula NGC 1514

Feibelman¹

1997

PASP

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Archival IUE low-dispersion spectra and the first ultraviolet high-dispersion spectrum of the binary nucleus of NGC 1514 have been analyzed. Both SWP and LWR low-dispersion spectra show variability by as much as a factor of two in the continuum level between the years 1978 and 1989. Weak P Cygni features for O v XI371 and C IV XI549 yield terminal wind velocities of -105 ±25 and -960 ±150kms -1 , respectively. No nebular emission lines were detected, but several photospheric and interstellar absorption features were observed. Absorption lines of Fe vn are suspected. The Hen XI640 absorption line has a radial velocity of +49±3 km s -1 and is in good agreement with optical data. The peculiar energy distribution of the SWP continuum for NGC 1514 can be synthesized by the coaddition of spectral-type A0-A3 III plus hot subdwarf IUE spectra.

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Section: Variabilitysupporting

confidence: 72%

The IUE Spectrum of the Binary Nucleus of the Planetary Nebula NGC 1514

Feibelman¹

1997

PASP

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“…The system is single-lined, so the masses of the other two components can only be guessed at. References: Mammano et al (1967); Gülmen et al (1985); Mayer (1990). Note: The O-C curve for this system displays a pronounced sinusoidal variation with a period of 3.78 yr.…”

Section: Details Of Individual Systemsmentioning

confidence: 88%

Eclipsing binaries in multiple-star systems

Chambliss

1992

PASP

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About 80 eclipsing binaries are known to be components of multiple-star systems. This is less than 2% of all known eclipsing-binary systems, but the actual total is certainly much higher than this, as the majority of stars under review are in fairly bright, well-studied systems. Triple-star systems are by far the most common of these, but one system in five is a quadruple or higher-order system. Quadruple systems include both systems of hierarchy 2 (two widely spaced pairs, e.g., BV+BW Draconis) and hierarchy 3 (e.g., r] Orionis). V772 Herculis and DN Ursae Majoris are in quintuple systems, and HR 3337 and the system that contains GZ Andromedae may also be quintuple. Castor, which contains the eclipsing binary YY Geminorum, is a very rare example of a sextuple-star system. Also considered are eclipsing binaries in compact star clusters such as SZ Camelopardalis and the two binaries in the Trapezium, BM Ori and V 1016 Ori. The most frequently encountered type of eclipsing binary to be found in multiple-star systems is that composed of two early-type (B5 or earlier) stars. Nearly all of the very close triple systems which have eclipsing-binary components are of this type. W UMa-type stars are also well represented among the multiple-star systems containing eclipsing binaries, but some other types are not. The RS Canum Venaticorum stars occur less frequently as components of multiple-star systems, and cataclysmic binaries appear to occur only very rarely as components of these systems. The physical and orbital properties of the multiple star systems are discussed in some detail in cases where the data are fairly complete, but it must be noted that many of the visual pairs have periods of revolution which are much too long to permit reliable determination of orbits. In triple-star systems with eclipsing binaries the ratio of P 2 /P x ranges from less than 10 (for A Tauri) to more than 10 7 in some cases. The questions of co-planarity of orbits and the membership of components in multiple-star systems are also considered.

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“…These are as follows: (i) The primary component of IM Aur was taken to be a B9 star according to Mammano et al (1967) and that is why its surface temperature was fixed at 10 500 K in GSG85. However, other studies give an earlier spectral type for the primary (e.g.…”

Section: New Light-curve Solutionmentioning

confidence: 99%

“…GSG85 obtained a mass ratio q = 0.32 employing the single-lined radial velocity curve obtained by Mammano et al (1967). Since this radial velocity curve is very undersampled and exhibits large scatter, we did not use it directly in our investigation.…”

Section: New Light-curve Solutionmentioning

confidence: 99%

Complex Period Variations in the Binary System IM Aurigae

Borkovits

Csizmadia

Hegedüs³

et al. 2002

A&A

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Abstract.Results of a new light-curve analysis and period variation study of the eclipsing binary IM Aur are presented. Four solutions are given according to the different spectral types of the primary, available in the literature. Multicolour photometry and the period analysis both indicate a close (≈0. 1) third physical member. If it is considered as a main-sequence star, then its spectral type is A2V-A8V, with a mass of m 3 ≈ 1.7−2.5 M . The light-time effect is modelled by the authors' simultaneous secular and periodic terms fitting code. Clear evidence of a secular period change is also revealed. The detailed effects of the perturbations by a third member of a close binary system are extensively studied, using one of the authors' latest numerical integrator code. Although the amplitudes of the expected O−C changes are too small and also the data set is far undersampled for clear confirmation of the theoretical expectation of the third body-perturbed eclipsing binary O−C curve, some typical patterns are shown for their possible identification amongst the O−C curves of other closer systems (like Algol, λ Tau) in the near future.

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Radial Velocity of the Central Star of NGC 1514

Cited by 3 publications

References 1 publication

The IUE Spectrum of the Binary Nucleus of the Planetary Nebula NGC 1514

The IUE Spectrum of the Binary Nucleus of the Planetary Nebula NGC 1514

Eclipsing binaries in multiple-star systems

Complex Period Variations in the Binary System IM Aurigae

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