The Eclipsing Variable HD 35921

Mayer, P.

doi:10.1086/128588

Cited by 8 publications

(3 citation statements)

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“…Besides the early RVs by Mayer (1968), RVs were also measured by Andersen et al (1974, hereafter ABH) on photographic spectra; they gave the ratio of the secondary and primary masses as q = m 2 /m 1 = 0.375. Stickland et al (1994) measured IUE spectra with the result q = 0.56.…”

Section: Spectroscopic Observations and Resultsmentioning

confidence: 99%

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The O-type eclipsing contact binary LY Aurigae – member of a quadruple system

Mayer

Drechsel²,

Harmanec

et al. 2013

A&A

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The eclipsing binary LY Aur (O9 II + O9 III) belongs to the rare class of early-type contact systems. We obtained 23 new spectra at the Ondřejov and Dominion Astrophysical Observatories, which were analysed with four older Calar Alto and one ELODIE archive spectra. A new result of this study is that the visual companion of LY Aur -the spectral lines of which are clearly seen in our spectra -is also an SB1 binary having an orbital period of 20.d 46, an eccentric orbit, and a radial velocity semi-amplitude of 33 km s −1 . The Hα line blend contains an emission component, which shows dependence on the orbital phase of the eclipsing system, with the strongest emission around the secondary eclipse. Revised elements of the eclipsing binary and the orbital solution of the companion binary are determined from our set of spectra and new light-curve solutions of the eclipsing pair. The mass of the primary of 25.5 M agrees well with its spectral type, whereas the secondary mass of 14 M is smaller than expected. From an O−C analysis of the minimum times of LY Aur that span more than 40 years, we found that the orbital period is decreasing, indicating the presence of interaction processes. The system is likely in a phase of non-conservative mass exchange.

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Section: Spectroscopic Observations and Resultsmentioning

confidence: 99%

“…The object LY Aur (HD 35921; ADS 4072A) was discovered as an eclipsing binary by Mayer (1968). Sota et al (2011) classified the binary as O9.5 II + O9 III.…”

Section: Introductionmentioning

confidence: 99%

The O-type eclipsing contact binary LY Aurigae – member of a quadruple system

Mayer

Drechsel²,

Harmanec

et al. 2013

A&A

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“…As noted above the disagreement between orbital semi-amplitude values determined from UV spectra and those from optical spectra -7is not unique to TU Mus. Four other massive semi-detached or contact systems have been spectroscopically studied in both the UV and optical: LY Aur (HD 35921, Stickland et al 1994;Mayer 1968;Andersen, Batten, & Hilditch 1974;Popper 1982), δ Ori A (HD36486, Harvin et al 2002), V Puppis (HD 65818, Stickland et al 1998Andersen et al 1983), andLZ Cep (HD 209481, Howarth et al 1991;Harries, Hilditch, & Hill 1998). All the Roche filling components have lower derived K values from the ultraviolet analysis when compared to the optical.…”

Section: Editor: Place Table 2 Herementioning

confidence: 99%

Tomographic Separation of Composite Spectra. XI. The Physical Properties of the Massive Close Binary HD 100213 (TU Muscae)

Penny¹,

Ouzts²,

Gies³

2008

ApJ

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We present the results of a Doppler tomographic reconstruction of the UV spectra of the double-lined, O-binary HD 100213 based on observations made with the International Ultraviolet Explorer (IUE). We used cross-correlation methods to obtain radial velocities, confirm the orbital elements, estimate the UV flux ratio, and determine projected rotational velocities. The individual component spectra are classified as O7 V + O8 V using UV criteria defined by Penny, Gies, & Bagnuolo. We present a model fit of the eclipsing light curve from observations from the HIPPARCOS satellite and published observations of Andersen

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