Some new spectroscopic binary orbits in NGC 6231 and SCO OB1.

Hill, Gary J.; Crawford, D. L.; Barnes, J. V.

doi:10.1086/111672

Cited by 42 publications

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“…Source C: Hill et al (1974) interchange the primary and secondary components compared to our nomenclature. The Julian dates which they give for a selection of Struve's spectra they used, denoted JD , are not heliocentric in fact.…”

Section: Spectroscopymentioning

confidence: 99%

“…However, since he could only observe the star near meridian from his location, he arrived at an incorrect period of 3 d .10. Hill et al (1974) .06. They derived new circular orbital elements, combining their and Struve's RVs and found a large difference in the γ velocities of the two binary components.…”

Section: Introductionmentioning

confidence: 99%

“…Tables 4 and 6 are available only in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/481/183 Levato & Morrell (1983) obtained two additonal RVs and by combining them with the velocities of Struve (1944) and Hill et al (1974) they derived a period of 5 d .89144 and an eccentric orbit. Using their period, Luna (1988) analysed his polarimetric observations of V1007 Sco and concluded that the orbital inclination had to be between 60…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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: Spectroscopymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

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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“…Radial velocity campaigns were led essentially by Struve (1944), Hill et al (1974), Levato & Morrell (1983), Levato et al (1988), Perry et al (1990), Penny et al (1994), Stickland & Lloyd (2001, IUE data), García & Mermilliod (2001), Sana et al (2002) and . Several authors also paid a special attention to particular objects, mainly binaries of which they performed a more detailed study.…”

Section: The Ngc 6231 Clustermentioning

confidence: 99%

An XMM-Newtonview of the young open cluster NGC 6231

Sana

Gosset

Rauw

et al. 2006

A&A

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This paper is the first of a series dedicated to the X-ray properties of the young open cluster NGC 6231. Our data set relies on an XMM-Newton campaign of a nominal duration of 180 ks and reveals that NGC 6231 is very rich in the X-ray domain too. Indeed, 610 X-ray sources are detected in the present field of view, centered on the cluster core. The limiting sensitivity of our survey is approximately 6 × 10 −15 erg cm −2 s −1 but clearly depends on the location in the field of view and on the source spectrum. Using different existing catalogues, over 85% of the X-ray sources could be associated with at least one optical and/or infrared counterpart within a limited cross-correlation radius of 3 at maximum. The surface density distribution of the X-ray sources presents a slight N-S elongation. Once corrected for the spatial sensitivity variation of the EPIC instruments, the radial profile of the source surface density is well described by a King profile with a central density of about 8 sources per arcmin 2 and a core radius close to 3.1 arcmin. The distribution of the X-ray sources seems closely related to the optical source distribution. The expected number of foreground and background sources should represent about 9% of the detected sources, thus strongly suggesting that most of the observed X-ray emitters are physically belonging to NGC 6231. Finally, beside a few bright but soft objects -corresponding to the early-type stars of the cluster -most of the sources are relatively faint (∼5 × 10 −15 erg cm −2 s −1 ) with an energy distribution peaked around 1.0-2.0 keV.

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“…The system has drawn much attention since the first description of Struve (1944). The first determination of the orbital period was based on the spectroscopic observations by Hill et al (1974) who found P = 2.446 ± 0.005 days. These authors reported a slightly eccentric (e = 0.07 ± 0.04) orbit and detected only spectral lines of the primary component with semi-amplitude K 1 = 162.5 ± 8.2 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

Photometric study of the eclipsing binary V1034 Sco

Bouzid

Sterken

Pribulla³

2005

A&A

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Abstract. We present multi-colour Strömgren photometry of the eclipsing binary V1034 Sco in the galactic open cluster NGC 6231, providing for the first time a full coverage of the orbital period (P = 2.44 days) and a complete analysis of the orbit. This extensive new photometry was analyzed together with multiband spectroscopy and results in an improved ephemeris, photometric elements and absolute parameters of the components. The system is close, but clearly detached. The masses of the components M 1 = 16.8 ± 0.5 M and M 2 = 9.4 ± 0.3 M do not correspond to the published spectral classification (O9III + B1III). The parameters of the components are consistent with the main-sequence luminosity class. We independently derive a distance modulus V 0 − M V = 10.73 ± 0.02.

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Some new spectroscopic binary orbits in NGC 6231 and SCO OB1.

Cited by 42 publications

References 0 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

An XMM-Newtonview of the young open cluster NGC 6231

Photometric study of the eclipsing binary V1034 Sco

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