The Active UV Phase of 59 Cyg

Doazan, V.; Grady, C.; Kuhi, L. V.; Marlborough, J. M.; Snow, Theodore P.; Thomas, R. N.

doi:10.1007/978-94-009-8565-0_66

Cited by 15 publications

(22 citation statements)

References 2 publications

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“…Only three SWP high-resolution IUE spectra of o Pup are available. The C iv and N v resonance lines show similar variations to those in 59 Cyg (Doazan et al 1985) or FY CMa (Peters et al 2008). Buscombe & Kennedy (1965) list o Pup as a star with variable radial velocity.…”

Section: Introductionmentioning

confidence: 63%

o Puppis: another Be+sdO binary?

Koubský

Kotková

Votruba

et al. 2012

A&A

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The spectrum of the Be star o Pup is shown to vary periodically with a period of 28.9 days. A radial-velocity variable He i 6678 Å emission component suggests that the star is the same type as φ Per, 59 Cyg, and FY CMa, i.e. binaries consisting of a Be star and a hot companion that illuminates the Be star disk (also called φ Per-type binaries or Be+sdO binaries). The range of radial-velocity variations of the stronger emission component in the helium line observed in o Pup is about 270 km s −1 , a value in good agreement with the range derived for φ Per-type binaries. The radial velocity curves defined by the prominent emission peak in He i 6678 Å line and Hα + Paschen emission move in anti-phase. We suggest that o Pup is generically similar to φ Per-type systems and may represent the fourth case of a Be star with a hot subdwarf companion.

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Section: Introductionmentioning

confidence: 63%

o Puppis: another Be+sdO binary?

Koubský

Kotková

Votruba

et al. 2012

A&A

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“…Note that our I V /I R ratio differs from the quantity denoted as V/R in the papers by Doazan et al (1985Doazan et al ( , 1989 which was defined as (I V − 1)/(I R − 1). It is necessary to warn that the Hα emission is so strong that in some profiles even a proper identification of the V and R peak of the emission is anything but easy.…”

Section: Spectroscopymentioning

confidence: 81%

“…Note that we also re-measured the 17 scanner Hα profiles obtained by Barker (1983) which were later included in the detailed study by Doazan et al (1985). Otherwise, we directly used the tabulated values from the papers by Doazan et al (1985Doazan et al ( , 1989 which we do not reproduce here.…”

Section: Spectroscopymentioning

confidence: 99%

“…The B1e star V832 Cyg (59 Cyg, HD 200120, BD+46 • 3133, HR 8047, f 1 Cyg, HIP 103632) is a wellknown Be star thanks to its very pronounced spectral variations, studied by Curtiss (1916), Duval et al (1975), Beeckmans (1976), Doazan et al (1980), Marlborough & Snow (1980), Divan & Zorec (1982), Barker (1982Barker ( , 1983, Doazan et al (1985) and Doazan et al (1989), among many others. Two short-lived shell phases were recorded in 1973 and in 1974-75.…”

Section: Introductionmentioning

confidence: 99%

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Properties and nature of Be stars

Harmanec

Božić

Percy³

et al. 2002

A&A

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“…2. Outflow models Several attempts were made to explain the origin of Be envelopes as a spheroidal outlow of gaseous material from the underlying star: the stellar-wind model by Gerasimovič (1934Gerasimovič ( , 1935, the variable mass flux model by Doazan & Thomas (1987) and Doazan (1987), the "bi-stable" or "axi-symmetric" radiation-driven wind model by Lamers & Pauldrach (1991), Araújo et al (1994) and Stee & Araújo (1994) and the wind-compressed disk model by Bjorkman & Cassinelli (1993) (see also the review by Bjorkman 2000). The latest one was considered as a very promising idea several years ago but the radiation-hydrodynamics simulations by Owocki et al (1996) showed that the small non-radial components in line forces inhibit formation of an equatorial disk by the windcompressed model.…”

Section: Attempts To Explain the Be Phenomenonmentioning

confidence: 99%

On the role of duplicity in the Be phenomenon

Harmanec

Bisikalo

Boyarchuk

et al. 2002

A&A

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Abstract. This paper begins a new series of studies devoted to a critical re-examination of the role of duplicity for the Be phenomenon and for the variability patterns observed for many Be stars. Based on both dynamical and energy considerations and a numerical gas-dynamical modelling, a new hypothesis of the formation of Be envelopes in binaries, via an outflow from a rapidly rotating B star in a detached binary, is outlined. It is shown that such an outflow is facilitated by the presence of a companion to the B star and leads to the formation of an envelope but not to any significant mass exchange between the binary components.

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The Active UV Phase of 59 Cyg

Cited by 15 publications

References 2 publications

o Puppis: another Be+sdO binary?

o Puppis: another Be+sdO binary?

Properties and nature of Be stars

On the role of duplicity in the Be phenomenon

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