Sixty four nights of <i>UBV</i> photometry of early‐type stars at La Sila

Mayer, P.; Božić, H.; Lorenz, R.; Drechsel, H.

doi:10.1002/asna.200911303

Cited by 11 publications

(21 citation statements)

References 30 publications

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“…Light variability was also reported by Feinstein & Ferrer (1968). Mayer et al (1992) indeed proved the eclipsing-binary nature of V1007 Sco and corrected the orbital period to 5 d .814. Their light curve clearly indicates a non-zero eccentricity because of unequal spacing between the primary and secondary minimum.…”

Section: Introductionsupporting

confidence: 56%

“…UBV observations obtained by Mayer et al (1992) which were added to the magnitude differences var-comp, were derived by us from a careful reduction of all observations including several standards using the HEC22 program -see Harmanec et al (1994) Very regrettably, neither of the comparisons but only V1007 Sco itself was observed by Hipparcos. These La Silla UBV observations of V1007 Sco and other early-type variables will be published in detail in a separate study (Mayer, in preparation).…”

Section: Photometrymentioning

confidence: 99%

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Improved estimates of the physical properties of the O-star binary V1007 Sco = HD 152248 and notes on several other binaries in the NGC 6231 cluster

Mayer

Harmanec

Nesslinger³

et al. 2008

A&A

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Context. In spite of the importance of massive O-type stars for astrophysics, their accurate masses and other fundamental properties are still a matter of debate. Determining them reliably is hampered by various factors (stellar winds and other forms of circumstellar matter), and the agreement of derived properties with the model predictions is far from satisfactory. Careful studies of O-type binaries, especially of those in stellar clusters, are therefore desirable. Aims. Having obtained new series of electronic spectra and UBV photometry of V1007 Sco, we analysed these data in an effort to check whether the observed properties of V1007 Sco indeed disagree with the prediction of stellar evolutionary models. We briefly analysed data for a few other binaries in NGC 6231, too. Methods. Spectral reductions were carried out with the MIDAS program, photometry reduced using the HEC22 program, the orbital elements were derived with the FOTEL program and the final solutions obtained with the program PHOEBE. Results. Our analysis led to an accurate determination of the apsidal advance,ω = (0.00884 ± 0.00012) deg d −1 , based on a simultaneous solution of all usable radial-velocity and photometric data. This implies an apsidal period of 111.5 years. It is also demonstrated that the orbital inclination must be close to 67• . We arrived at the following preliminary values for masses and radii: M 1 = (29.5 ± 0.4) M , M 2 = (30.1 ± 0.4) M , R 1 = (15.8 ± 0.7) R , and R 2 = (15.3 ± 0.5) R . These values clearly indicate a log g of about 3.5 [CGS], implying that the stars are giants and not supergiants, as the standard spectral classification criteria indicate.

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Section: Introductionsupporting

confidence: 56%

Section: Photometrymentioning

confidence: 99%

Improved estimates of the physical properties of the O-star binary V1007 Sco = HD 152248 and notes on several other binaries in the NGC 6231 cluster

Mayer

Harmanec

Nesslinger³

et al. 2008

A&A

Self Cite

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“…4 away. This appears to be just a simple misidentification, as reported by Mayer et al (1992). Lines used in model fitting included the wings of Hδ and Hγ , He i λ4471, 4713, and He ii λλ4541, 4686.…”

Section: Cpd-59mentioning

confidence: 76%

Radial Velocities of Galactic O-Type Stars. I. Short-Term Constant Velocity Stars

Gies

Hillwig

McSwain

et al. 2011

The Astronomical Journal

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“…With a combined magnitude of V = 6.45, HD 101205 is a visual binary with a separation of 0.36 arcsec and Δ V = 0.3 (Mason et al 1998). It is also the brightest source in the cluster and a known eclipsing system with a period of 2.1 d (Balona 1992; Mayer, Lorenz & Drechsel 1992; Otero 2007). Additional photometry (Mayer et al 2010) reveals however a more complicated light curve than expected for an eclipsing binary suggesting that the true nature of the system is not fully understood.…”

Section: O‐type Stars In Ic 2944mentioning

confidence: 99%

The massive star binary fraction in young open clusters - III. IC 2944 and the Cen OB2 association

Sana

James²,

Gosset³

2011

Monthly Notices of the Royal Astronomical Society

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Using an extended set of multi‐epoch high‐resolution high signal‐to‐noise ratio optical spectra, we readdress the multiplicity properties of the O‐type stars in IC 2944 and in the Cen OB2 association. We present new evidence of binarity for five objects and we confirm the multiple nature of another two. We derive the first orbital solutions for HD 100099, HD 101436 and HD 101190 and we provide additional support for HD 101205 being a quadruple system. The minimal spectroscopic binary fraction in our sample is fmin= 0.57. Using numerical simulations, we show that the detection rate of our observational campaign is close to 90 per cent, leaving thus little room for undetected spectroscopic binary systems. The statistical properties of the O‐star population in IC 2944 are similar, within the uncertainties, to the results obtained in the earlier papers in this series despite the fact that sample size effects limit the significance of the comparison. Using newly derived spectroscopic parallaxes, we reassess the distance to IC 2944 and obtained 2.3 ± 0.3 kpc, in agreement with previous studies. We also confirm that, as far as the O stars are concerned, the IC 2944 cluster is most likely a single entity.

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Sixty four nights of UBV photometry of early‐type stars at La Sila

Cited by 11 publications

References 30 publications

Improved estimates of the physical properties of the O-star binary V1007 Sco = HD 152248 and notes on several other binaries in the NGC 6231 cluster

Improved estimates of the physical properties of the O-star binary V1007 Sco = HD 152248 and notes on several other binaries in the NGC 6231 cluster

Radial Velocities of Galactic O-Type Stars. I. Short-Term Constant Velocity Stars

The massive star binary fraction in young open clusters - III. IC 2944 and the Cen OB2 association

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